International Symposium & Summer School on
Planetary Science (IAPS 2013)
July 1-7, 2013, Shanghai, China http://202.127.29.4/meetings/iaps2013; http://202.127.29.4/schools/school2013
Venue: 3rd floor of Astronomical Building Shanghai Astronomical Observatory, Chinese Academy of Sciences
International Symposium on
Planetary Sciences (IAPS2013) July 1-4, 2013, Shanghai, China
http://www.shao.ac.cn/meetings/iaps2013
Contact Information:
Email: [email protected]; [email protected]
Emergency Phone: 13918401214
Police: 110; Ambulance: 120
Venue: 3rd
floor, Astronomical Building
Shanghai Astronomical Observatory, Chinese Academy of Sciences
80 Nandan Road, Shanghai 200030, China
Available WIFI at the workshop with the password at conference hall doors
Sponsors
International Association of Planetary Sciences (IAPS)
Shanghai Astronomical Observatory (SHAO), CAS
Key Lab for Planetary Science of Chinese Academy of Sciences
National Basic Research Program of China (973 Program)(2012CB72000)
China University of Geosciences at Wuhan (CUG)
International Association of Geodesy (IAG) SC2.6 & SC4.6
Steering Committee
Shuhua Ye (SHAO, China) (Chair)
Scientific Organizing Committee (SOC)
Ricardo Amils (UAM, Spain)
Oliver Baur (OEAW, Austria)
Kwing Lam Chan (UST, Hongkong)
Athena Coustenis (OBSPM, France)
Pingyuan Cui (BIT, China)
Alexander Gusev (KFU, Russia)
Joern Helbert (DLR, Germany)
Wing-Huen Ip (NCU, Taiwan)
Shuanggen Jin (SHAO, CAS, China) (Chair)
Rafael.Kascheev (KFU, Russia)
Tatsuaki Okada (ISAS/JAXA, Japan)
Ziyuan Ouyang (NAOC, China)
Gerald Schubert (UCLA, USA)
Vlad. Shevchenko (MSU, Russia) (Co-Chair)
Oleg Titov (Geoscience, Australia)
Vyacheslav Turyshev (JPL, USA)
Long Xiao (CUG, Wuhan, China)
Roger Yelle (Uni. Arizona, USA)
Eliot F. Young (SWRI, USA)
Ji-Lin Zhou (NJU, China)
Local Organizing Committee (LOC)
Wenli Dong (SHAO)
Guiping Feng (SHAO)
Shuanggen Jin (SHAO) (Chair)
Rui Jin (SHAO)
Xuerui Wu (SHAO)
Yansong Xue (SHAO)
Tengyu Zhang (SHAO)
Topics
Planetary probes navigation and control (Pingyuan Cui, Ji-Lin Zhou)
Planetary Geodesy and Gravity field (Rafael.Kascheev, Oliver Baur)
Atmosphere & ionosphere of terrestrial planets (Eliot F. Young, Shuanggen Jin)
Planetary systems, Rotation and Fluid dynamics (Ji-Lin Zhou, Gerald Schubert)
Science and Exploration of the Moon (Vladislav V. Shevchenko, Kwing Lam Chan)
Science and Exploration of Mars (Alian Wang, Long Xiao, Varun Sheel)
Science and Exploration of Venus (Eliot F. Young, Wing-Huen Ip)
Science and Exploration of the Mercury (Joern Helbert, Kwing Lam Chan)
Comparative and Laboratory Planetary Sciences (Long Xiao, Yangtin Lin)
Planetary Life and Astrobiology(Athena Coustenis, Ricardo Amils )
Giant and Extrasolar Planets Sciences(Roger Yelle, Shuanggen Jin)
Future Planetary Missions & Instrumentations (Tatsuaki Okada, Eliot F. Young)
Invited Sessions
1. Rotational motion and inner dynamics of the Earth, Mars and Moon
Conveners: Yury Barkin (Russia), Hideo Hanada (Japan), Koji Matsumoto (Japan), S. Sasaki, Jose
Ferrandiz (Spain).
2. New GNSS, VLBI and Laser Ranging Technologies for Lunar and Planetary Science
Conveners: Vyacheslav Turyshev (USA), Oleg Titov (Australia), Alexander Gusev (Russia)
3. Planetary Remote Sensing and Geoinformatics
Conveners: Siddan Anbazhagan (India), Kaichang Di (China).
4. Planetary Environments and Solar wind interaction
Conveners: Susan Mckenna-Lawlor (Ireland).
5. Asteroids and comets exploration and science
Conveners: Jianghui Ji (China), Maria Teresa Capria (Italy).
6. Dynamics of planetary rings and circumplanetary dust
Conveners: Juergen Schmidt (Finland).
7. Exploration of Planetary Systems and Their Habitability
Conveners: Padma Yanamandra-Fisher (USA).
8. Laboratory work in support of planetary missions
Conveners: Joern Helbert (Germany).
9. Poster-Discussion Session: Imbalance of Nature in Space
Main Convener and Chair: Vladimir Kontar (USA).
Free Open Oral Forum-Discussion and Brainstorm: “Imbalance of Nature”
Main Convener and Chair: Vladimir Kontar (USA).
Full papers for the Book:
Planetary Exploration and Science: Recent Advances and Applications, Springer Verlag, Heidelberg,
Germany
Deadline of full paper submission: August 31, 2013
Dear All Participants
The International Symposium and Summer School on Planetary Sciences (IAPS2013) will be held at the
Shanghai Astronomical Observatory, Chinese Academy of Sciences, July 1-7, 2013, Shanghai, China, which
brings together international scientists to present and discuss the latest results on exploration and science of
Mercury, Venus, Earth, Moon, Mars, Saturn, Jupiter..., and seeking life beyond Earth. Topics include
Planetary geodesy, navigation, remote sensing, atmosphere, ionosphere/plasma physics, magnetic and gravity
field, geomorphology, geophysics, geology, petrology, geochemistry, interior physics, Life & Astrobiology,
Giant & Extrasolar Planets, etc.
On behalf of the Organizing Committee, we are pleased to invite you to attend the International Symposium
and Summer School on Planetary Science, July 1-7, 2013, Shanghai, China. For any questions, please feel free
to contact LOC at http://202.127.29.4/meetings/iaps2013; http://202.127.29.4/schools/school2013
Sincerely yours
Prof. Shuanggen Jin
On behalf of the Organizing Committee,
Astronomical Building of Shanghai Astronomical Observatory, CAS
25m radio telescope, 1.56m reflector, SLR, GPS etc. at SHAO
1. Symposium Program Schedule
Monday 1
st July 2013
10:00-17:00 Registration (Third floor of SHAO)
Tuesday 2
nd July 2013
08:00-17:00 Registration (Third floor of SHAO)
08:50-09:00 Opening Ceremony (Room A)
Chair: Shuanggen Jin
09:00-10:30 Panel Session 1 (Room A)
Chair: Athena Coustenis, Joern Helbert
09:00-09:30 Gravity Field and Tides of Titan (INVITED)
Luciano Iess (Uni Rome, Italy)
09:30-10:00 A simulation study for constraining the lunar internal structure by geodetic and seismic data(INVITED)
Koji Matsumoto (NAOJ, Japan)
10:00-10:30 China Deep-Space Exploration: Progresses and Future Thoughts(INVITED)
Jiangchuan Huang (China Acad. Space Tech., China)
Take Group Photo at first floor & Coffee Break
10:50-12:40 Panel Session 2 (Room A)
Chair: Roger Yelle, Kwing Lam Chan
10:50-11:20 Planetary Evolution and Life: Astrobiology from a Planetary Science Perspective (KEYNOTE)
Tilman Spohn (DLR, Germany)
11:20-11:50 Habitable Extrasolar Planets: Formation, Observations and Challenges (INVITED)
Nader Haghighipour (Hawaii University, USA)
11:50-12:20 Japanese atmospheric escape mission to Mars (heir of NOZOMI): Role of atmospheric escape in
evolution of Martian environment(INVITED)
Kanako Seki (Nagoya University, Japan)
12:20-12:40 Panel discussion (Luciano Iess, Kanako Seki, Koji Matsumoto, Jiangchuan Huang, Tilman Spohn, Nader
Haghighipour)
Lunch (Cafeteria, 2
nd floor of Active Center Building)
14:00-15:40 Session 1: Science and Exploration of the Moon (Room A)
Chair: Koji Matsumoto, Hauke Hussmann,
14:00-14:20 Oliver Baur , GRAIL lunar gravity field recovery: simulation studies and first real data results
14:20-14:40 Zongyu Yue, One possible origin of olivine in Copernicus crater: the remnants of projectile
14:40-15:00 Bo Wu, Integration of Chang’E-2 Imagery and LRO Laser Altimeter Data for Precision Lunar Topographic Modeling
and Analysis
15:00-15:20 Yuji Harada, Frequency-dependence of the tidal dissipation on the Moon: Effect of the low-viscosity zone at the
lowermost mantle
15:20-15:40 Kaichang Di, A new lunar global DEM derived from Chang’E-1 Laser Altimeter data with crossover adjustment
(INVITED)
Coffee Break
15:50-17:40
Session 2A: New Technologies for Lunar and
Planetary Science (Room A)
Chair: Kaichang Di, Shengbo Chen
Session 2B: Rotational motion and inner
dynamics of the Planet Earth (Room B)
Chair: Wenbin Shen, Robert Tenzer
15:50-16:10 Marco Gregnanin, CDMA-Based Same Beam
Interferometry for Future Deep Space Missions Wenbin Shen, New estimate of the present Earth
expansion based on geodetic observations
16:10-16:25 Lian Yi , The Analysis on abnormal brightness temperature
in lunar south pole by SVD method based on Chang’E-2
MRM data
Wenbin Shen, Theoretical prediction and observation
evidences on the northward drift and annual
oscillation of the Earth’s core from space geodesy
16:25-16:40 Yu He, A method of Image Matching Based on Lunar Image
Leonid Zotov , Influence of the atmosphere and ocean
on the resonant polar motion
16:40-16:55 Ming Ma, Analysis on lunar thermal infrared emissivity
spectral features: application to the Diviner Lunar
Radiometer data
Robert Tenzer , Gravimetric forward and inverse
modeling methods for global recovery of the crustal
density structures and crust-mantle interface
16:55-17:10 Misha Barkin, The forced and free physical libration of the
Moon with ellipsoidal liquid core and elastic mantle
Erhu Wei, Fitting the Sure-part of Polar Motion with
Two-frequency Phenomenon of Chandler Wobble
17:10-17:25 Rui Zhang, Research and Application of the "Compass"
Single-frequency Data High-precision Processing
Technology
Erhu Wei, Combining and predicting of Earth
Rotation Parameters
17:25-17:40 Alexander Gusev, VLBI Astrometry, Rotation, Physical
Libration and Interior Structure of the Moon for
"LUNA-GLOB" and "LUNA RESOURCE" Russian space
missions(2015-2017yrs)"
Tomas Ignacio Gomez , Temporary evolution of the
center of timing and average annual stream flow
projections for the 21st century in a Chilean
central-located Adnean basin
18:30-21:00 Banquet (5th
floor, Ronggang Restaurant)
Wednesday 3nd July 2013
08:30-10:30 Session 3A: Planetary probes navigation and
control (Room A)
Chair: Mau Wong, Pingyuan Cui, Erhu Wei
Session 3B: Science and Exploration of the
Moon (Room B)
Chair: Oliver Baur, Qin Xu,
08:30-08:45 Ruoyan Wei , An approach based on shadow areas matching
for visual navigation in planetary landing
Jinjin Zhao, Morphology Analysis of Lunar Craters
Based on Multi- Source Data
08:45-09:00 Wei Shao, Error Characterization of Vision-based Detection
and Tracking for Spacecraft Navigation
Yunlong Lin, Calculations of the Lunar Surface
Electrical Field for the Estimations of Moon Dust and
its Distributions for Future Lunar Explorations
09:00-09:15 Mau C. Wong, Mars Science Laboratory Trajectory and
Maneuver Analyses
Man Peng, Multiple Image Shape-From-Shading for
Detailed Lunar Terrain Mapping Using Chang’E
Images
09:15-09:30 Yunzhang Wu, Robust Three-Stage Kalman filter for the
Navigation during Mars Entry
Qian Huang, Density and Elastic thickness
constraints of lunar large shield volcanos from gravity
and topography
09:30-09:45 Maodeng Li, Navigation Fusing a Single Optical
Observation with a Single Pulsar Based on Observability
Analysis
Sahnggi Park , An optical experiment to measure a
torque acted by the Moon on the Earth equator
09:45-10:00 Taishan Lou , Considering Uncertain Parameter in the Pengju Guo, Topographic Correction based Retrieval
Dynamic systems during Mars Entry of Lunar Clinopyroxene Abundance from M3 Data
10:00-10:15 Yunzhang Wu, Two-Stage Extended Kalman Filter applied
to powered descent phase of Mars EDL
Linzhi Sun, Lunar Global Iron Mapping with Partial
Least Squares Regression 10:15-10:30 Qunshan Shi, Landing area terrain reconstruction method
combined laser rangefinder
Erhu Wei, Joint GNSS and SLR Data for the Study of
Earth Rotation Parameters
Coffee Break
10:40-12:35 Session 4: Planetary Life and Astrobiology (Room A)
Chair: Tilman Spohn, Junichi Watanabe
10:40-11:10 Nader Haghighipour, Detecting Earth-like planets and water origin(INVITED)
11:10-11:30 Junichi Watanabe, Jovian Impact Flashes and their Implication to Small Solar System Bodies (INVITED)
11:30-11:50 Mau C. Wong, Molecular-Kinetic Simulations of Escape from The Ex-Planet and Exoplanets: Criterion for Transonic
Flow
11:50-12:20 Athena Coustenis, Icy moons as habitable worlds and their exploration
12:20-12:35 Yanqiu Li, Comparison among different lunar surface ages calculation methods by lunar crater frequency-size
distribution
Lunch (Cafeteria, 2
nd floor of Active Center Building)
14:00-15:30 Session 5: Planetary Environments and Solar wind interaction (Room A)
Chair: Wojcieh Markiewicz, Miriam Rengel
14:00-14:30 Kanako Seki, Effects of the surface conductivity and IMF strength on dynamics of planetary ions in Mercury’s
magnetosphere(INVITED)
14:30-14:50 Nishant Arora, Space debris: Its alarming state
14:50-15:10 Shuanggen Jin, Variations and fluctuations of the Venusian bow shock from Venus Express MAG and ASPERA-4
observations(INVITED)
15:10-15:30 Robert Rankin , Global Hybrid Kinetic Simulations and Comparison with MESSENGER
Coffee Break
15:40-17:40 Session 6: Science and Exploration of Mars (Room A)
Chair: Kanako Seki, Giuseppe Piccioni
15:40-16:00 Qin Xu, Harris Operator Feature Point Matching for Sequence Image of Mars
16:00-16:20 Yansong Xue, Minerals and rock components recognition at Martian Gale region from MRO CRISM hyperspectral
images
16:20-16:40 N. A. Chujkova , Anomalies of density, stress and gravity in the interior of Earth and Mars and possible geodynamical
consequences: A comparative analysis
16:40-17:00 Tengyu Zhang, Automatic recognition of impact craters on Mars based on DEM data
17:00-17:20 Xiaohua Fang, Understanding The Importance of Pickup Oxygen Ion Precipitation to the Mars Upper Atmosphere
17:20-17:40 Xun Geng , Analysis of Epipolar Line for Mars Express HRSC Linear Pushbroom
19:00-21:00 Project Meeting (Room B)
Thursday 4
th July 2013
08:30-10:30 Session 7: Giant and Extrasolar Planets Sciences (Room A)
Chair: Ji-lin Zhou, Nader Haghighipour
08:30-09:10 Paul Hartogh, Did comets deliver water to Earth? (INVITED)
09:10-09:30 Victor Tejfel , Probable signs of the clouds vertical inhomogeneity on Jupiter
09:30-09:50 Su Wang, Predicting the mean motion resonance formation in the Kepler observed systems
09:50-10:10 Liyun Zhang, The follow-up observations of several exoplanet transit events
10:10-10:30 Roger Yelle , Structure and Escape of Extrasolar Planet Upper Atmospheres
Coffee Break
10:40-12:20 Session 8: Exploration and Science of Venus (Room A)
Chair: Luciano Iess, Robert Rankin
10:40-11:00 Wojcieh Markiewicz , Venus upper clouds; morphology, dynamics and physical properties(INVITED)
11:00-11:20 Jianguo Yan, A refined gravity field model of Venus VGM2013 using high resolution topography data
11:20-11:40 Giuseppe Piccioni, A review of the main results from the VIS-IR imaging spectrometer VIRTIS on board Venus
Express(INVITED)
11:40-12:00 Miriam Rengel, Tracing the CO composition and winds in Venus s atmosphere at the submillimetre wavelengths:
Advances(INVITED)
12:00-12:20 Misha Barkin, Unified theory of planetary processes of planets, satellites and the Sun
Lunch (Cafeteria, 2nd
floor of Active Center Building)
14:00-15:40 Session 9A: Asteroids and comets exploration
and science (Room A)
Chair: Jianghui Ji, Maria Teresa Capria
IAPS Meeting (Room B)
(SOC members and Invited Speakers)
14:00-14:20 Maria Teresa Capria , Dawn at Vesta: picture of a
protoplanet(INVITED)
14:20-14:40 Yuhui Zhao, A Method to Compute Gravitational
Harmonic Coefficients of Irregular Small bodies
14:40-15:00 Chaozhen Lan, 3D Reconstruction of Vesta From
Sequence Image of DAWN Based on Multi-view dense
Matching Algorithm
15:00-15:20 Eleonora Ammannito , Vestan lithologies mapped by the
Visual and Infrared Spectrometer on Dawn
15:20-15:40 Yao Dong, Tidal evolution of the Kepler-10 system
Coffee Break
15:50-17:40 Session 10: Future Planetary Missions & Instrumentations (Room A)
Chair: Paul Hartogh, Sanjay Limaye
15:50-16:10 Sanjay Limaye , Case for Future Exploration of Venus(INVITED)
16:10-16:30 Kwing Lam Chan , Proposal for a Mission to Uranus
16:30-16:50 Joern.Helbert, MERTIS on BepiColombo - seeing Mercury in a new light
16:50-17:10 Hauke Hussmann, Exploration of the Galilean Satellites: The Ganymede Laser Altimeter (GALA) on-board the
JUICE Mission(INVITED)
17:10-17:40 Discussion and Farewell
18:30-21:00 Dinner at Heji Restaurant (SOC Members & Session Chairs)
Posters
Name Affiliation Title
Naveen
Chandra Indian Ins. Tech.
Integration of spatial and spectral information for endmember
extraction and subspace identification for hyper spectral data
Robert Tenzer Wuhan Univ. Signature of the ocean-floor spreading, hot spots, and subducted slabs
in marine gravity data
Robert Tenzer Wuhan Univ. Empirical density model of marine sediments
Erhu Wei Wuhan Univ. On the Relationship between the Change of Earth Rotation Rate and
Earthquake
Sun Kwok Hong Kong Univ. Stellar synthesis of organic compounds and their effects on the early
solar system
Anil
Bhardwaj PRL, India
Interaction of Solar Wind with the Moon: A New View from the
SARA/Chandrayaan-1
G.
Kochemasov IGEM, Russian Acad. of Sci., Russia
The Moon: collars of beads in and around the Mare Orientale make
questionable its widely cited impact origin
Yuji Harada CUG A time scale of true polar wander on a quasi-fluid planet: Effect of a
low-viscosity layer inside a mantle
2. Summer School Schedule
Time Dates
Friday 5th July 2013
09:00-09:10 Opening Ceremony
09:10-09:30 Introduction of SHAO and Lecturers
09:30-10:30 Shuanggen Jin (SHAO, China) - Space Geodesy & Applications
Take Group Photo & Coffee Break
10:50-12:00 Shuanggen Jin (SHAO, China) - Planetary Geodesy & Science
12:00-12:20 Questions & Discussion
Lunch
14:00-15:30 Athena Coustenis (Paris Observ., France) - Exploration of the Outer Solar System
Coffee Break
15:50-17:10 Athena Coustenis (Paris Observ., France) - Exploration of the Outer Solar System
17:10-17:40 Questions & Discussion
18:00-20:00 Party
Saturday 6th July 2013
08:30-10:00 Paul Hartogh (MPS, Germany) - Remote Sensing of Solar System Objects
Coffee Break
10:20-11:50 Paul Hartogh (MPS, Germany) - Remote Sensing of Solar System Objects
11:50-12:20 Questions & Discussion
Lunch
14:00-15:30 Luciano Iess (Uniroma, Italy) - Radio Science for Planetary Geodesy
Coffee Break
15:50-17:10 Luciano Iess (Uniroma, Italy) - Radio Science for Planetary Geodesy
17:10-17:40 Questions & Discussion
17:30-19:00 Reception
Sunday 7th
July 2013
08:30-10:00 Hauke Hussmann (DLR, Germany) - Planetary Altimetry and Dynamics
Coffee Break
10:20-11:50 Hauke Hussmann (DLR, Germany) - Planetary Altimetry and Dynamics
11:50-12:20 Questions & Discussion
Lunch
14:00-15:30 Koji Matsumoto (NAOJ, Japan) - Lunar gravity field modeling
Coffee Break
15:50-17:10 Koji Matsumoto (NAOJ, Japan) - Lunar gravity field modeling
17:10-17:40 Questions & Discussion
3. Abstract
Gravity Field and Tides of Titan
L. Iess
Dipartimento di Ingegneria Meccanica e Aerospaziale
Sapienza Università di Roma, Italy
Since its gravitational capture on July 1st, 2004, the Cassini spacecraft carried out a wealth of
observations of Saturn and its moons. Titan, being at the same time one of the main goals and the
true engine of the mission, has been encountered more than 90 times. The interior structure of the
satellites, crucial to the understanding of the formation processes of the Saturnian system, has been
investigated mainly with gravity measurements enabled by precision tracking of the spacecraft from
ground antennas. The seven flybys devoted to gravity science provided the determination of a full
3x3 gravity field, dominated by largely hydrostatic quadrupole harmonics. The Radau-Darwin
approximation indicates a relatively large moment of inertia factor (0.34) and likely a partially
differentiated structure. The good accuracy of range rate data allowed also the measurement of the k2
Love number, controlling the variable part of the quadrupole field. The large value of k2 (0.59 +/-
0.16, 2-sigma) indicates the presence of large tidal deformations on Titan and provides a compelling
evidence of an internal ocean under the thick, outer icy shell. The combination of space geodetic and
radar altimetric measurements provides further insight on the features of the outer shell. This talk
reviews the main results obtained so far in the geodesy of Titan and outlines their relevance to the
exploration of the Jovian moons by ESA’s JUICE mission.
Icy moons as habitable worlds and their exploration
A. Coustenis 1, A. Solomonidou
1,2, Th. Encrenaz
1, O. Grasset
3, F. Sohl
4, H. Hussmann
4, F. W.
Wagner 4, F. Raulin
5, D. Schulze-Makuch
6
1 LESIA - Observatoire de Paris, CNRS, UPMC Univ. Paris 06, Univ. Paris-Diderot –Meudon, France,
2 National
and Kapodistrian University of Athens, Department of Geology and Geoenvironment, Athens, Greece 3 Lab. Planet. & Geodyn. Nantes, France
4 DLR, Institute of Planetary Research, Berlin, Germany
5 LISA-IPSL, CNRS/UPEC & Univ. Paris Diderot, Créteil, France
6 Washington State University, School of Earth and Environmental Sciences, Washington, USA.
Abstract: The study of the habitable conditions in the outer solar system tends to enlarge the limits of
the traditional habitable zone. Several of the icy moons show such promising conditions for the
development and/or maintenance of life. Jupiter’s Europa, Callisto and Ganymede as well as
Saturn’s Titan and Enceladus, seem to satisfy many of the “classical” criteria for habitability such as
the presence of liquid water, the energy sources to sustain metabolism and the “nutrients” over a
period of time long enough to allow the development of life. Cassini-Huygens demonstrated that
Titan and Enceladus possess active organic chemistries subject to seasonal variations and unique
geological features. Additionally, all these satellites show indications of harboring liquid water
oceans under their icy crusts, which may even be (in the case of Europa) in direct contact with a
silicate mantle floor and kept warm through time by tidally generated heat. Such evidence suggests
that habitability conditions can be found not only on the surfaces of Earth-like planets, but in
far-away objects in their interiors. Furthermore, the strong gravitational pull caused by the giant
planets may produce enough energy to sufficiently heat the cores of orbiting icy moons. Similarly,
waterworlds can exist in exoplanets which are currently investigated thoroughly from large
ground-based telescopes and earth observatories. In the solar system, such potential habitats can be
investigated with designated space missions, like ESA’s JUpiter ICy moon Explorer to Jupiter’s
system (launch in 2022). Titan could be explored in the future via mission concepts like TSSM or
TiMe which have been studied by the space agencies.
A Method to Compute Gravitational Harmonic Coefficients of
Irregular Small bodies
Zhao Yuhui1 Wang Su
1 Ji Jianghui
1
1Purple Mountain Observatory Chinese Academy of Science
Abstract: During the orbit design procedure of the small bodies’ exploration missions, it’s important
to take the effect of the gravitation of the small bodies into account. However, a majority of the small
bodies in the solar system are irregularly shaped with nonuniform density distribution which makes it
difficult to precisely calculate the gravitation of these bodies.
This paper proposes a method to model the gravitational field of an irregularly shaped small body
and calculate the corresponding spherical harmonic coefficients. This method is based on the shape
of the small bodies resulted from the light curve data via observation, and use finite volume element
to approximate the body shape. According to the definition of spherical harmonic parameters, it
could be derived numerically by computing the integral straight.
Take the asteroid Eros433 for example, spherical harmonic coefficients resulted from this method is
compared with the result derived from track data obtained by NEAR detector, the comparison show
that the maximum error is less than 6%. Comparison with the conventional triaxial ellipsoid model
and polyhedron method shows that this method applies to uneven density distribution objects. It
could be used to provide reliable gravity field data of small bodies for orbit design and landing in the
exploration missions.
Keyword: Small bodies, irregularly shaped gravity field, spherical harmonics parameters
A simulation study for constraining the lunar internal structure by
geodetic and seismic data
Koji Matsumoto1, Ryuhei Yamada
1, Fuyuhiko Kikuchi
1, Sander Goossens
2, Shunichi Kamata
3, Takahiro Iwata
4,
Hideo Hanada1, Yoshiaki Ishihara
5, Sho Sasaki
6
1 National Astronomical Observatory of Japan,
2 NASA Goddard Space Flight Center
3 Hokkaido University,
4 JAXA,
5 AIST, 6 Osaka University
Abstract: Internal structure and composition of the Moon provide important clue and constraints on
theories for how the Moon formed and evolved. The Apollo seismic network has contributed to the
internal structure modeling. Efforts have been made to detect the lunar core from the noisy Apollo
data, but there is scant information about the structure below the deepest moonquakes at about 1000
km depth. On the other hand, there have been geodetic studies to infer the deep structure of the Moon.
For example, LLR (Lunar Laser Ranging) data analyses detected a displacement of the lunar pole of
rotation, indicating that dissipation is acting on the rotation arising from a fluid core. Bayesian
inversion using geodetic data (such as mass, moments of inertia, tidal Love numbers k2 and h2, and
quality factor Q) also suggests a fluid core and partial melt in the lower mantle region. Further
improvements in determining the second-degree gravity coefficients (which will lead to better
estimates of moments of inertia) and the Love number k2 will help us to better constrain the lunar
internal structure. Such improvements will be made by future lunar missions including Japanese
SELENE-2. A preliminary simulation study shows that the k2 accuracy of better than 1% is
anticipated by the SELENE-2 differential VLBI mission for which one of the radio sources is fixed
on the moon serving as the reference to determine the orbiter’s trajectory.
We carried out a feasibility study using Bayesian inversion on how well we can constrain the lunar
internal structure when such improvements are made on the geodetic data. It is difficult to tightly
constrain the internal structure from the geodetic data only because there are trade-offs among crust,
mantle, and core structures. However, when combined with the existing Apollo seismic data which
constrain the structures of crust and mantle, such geodetic data will contribute to narrow the range of
the core structure models. A result with 5-layer model shows that the size of the fluid core can not be
determined well with the current error level of the geodetic data, but can be determined with an
accuracy of about 10% when 1% of k2 accuracy is achieved. The impact of the crustal structure
uncertainties on the estimation of the core size is relatively small. The determination of the core
density is more difficult, since the ratio of fluid core moment to total moment is of the order of 10-3
.
The Analysis on abnormal brightness temperature in lunar south
pole by SVD method based on Chang’E-2 MRM data
Lian Yi ,Chen Sheng-bo ,Meng Zhi-guo,Guo Peng-ju,Li Yan-qiu
College of Geoexploration Science and Technology,
Jilin University, Changchun 130026
Email:[email protected]
Abstract: Interests in the Moon start to increase recently, and henceforth, more and more attention
has been paid to the heat resources and the water ice in the lunar south pole. This paper uses
Chang’E-2 microwave radiometer (MRM) data to calculate the hour angle by the transformation
between the horizon coordinate system and the lunar equatorial coordinate system. The brightness
temperature(TB) data in south pole at different times in the different channel would be obtained by
kriging interpolation.We discuss the relationship between TB for 37GHz channel and TB for 3GHz
channel in one day at noon, and use singular value decomposition(SVD) method to analyse abnormal
brightness temperature. An analysis by the SVD method provides the intra class correlation diagram
for 37GHz channel which shows abnormal brightness temperature in lunar surface and the
heterogeneous correlation diagram shows the influence of TB for 3GHz channel to TB for 37GHz
channel. The cold anomalous point may be the permanent shadow areas in lunar south pole and the
thermal anomalous point may have sufficient resources of heat by analyzing the intra class
correlation diagram. The heterogeneous correlation diagram was used to detect the areas whether
water ice exists.
Key words: Lunar south pole, SVD, water ice, Hour angle, Brightness temperature
Did comets deliver water to Earth?
P. Hartogh1, D.C. Lis
2, D. Bockelée-Morvan
3, M. de Val-Borro
1, N. Biver
3, M. Küppers
4, M.
Emprechtinger2, E.A. Bergin
5, J. Crovisier
3, M. Rengel
1, R. Moreno
3, S. Szutowicz
6, G. A. Blake
2
and the HssO-team
1 Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany,
[email protected] 2 California Institute of Technology, Pasadena, CA, USA
3 LESIA Observatoire de Paris, CNRS, UPMC, Université Paris-Diderot, France
4 Rosetta Science Operation Centre, European Space Astronomy Centre, Madrid, Spain
5 Astronomy Center, University of Michigan, Ann Arbor, USA
6 Space Research Centre, Polish Academy of Sciences, Warsaw, Poland
Abstract: For decades, the source of Earth volatiles, especially water, has been a subject of debate.
Proposed explanations include accretion of material in the vicinity of the Earth orbit or delivery by
impacts of asteroids or comets during the late heavy bombardment (LHB). The source of water
reservoirs can be accurately traced by measurements of the deuterium-to-hydrogen isotopic ratio
(D/H). Previous measurements of this ratio in several Oort cloud comets resulted in a value twice as
high as that in the Earth oceans, leading to the generally accepted conclusion that comets are unlikely
to be the primary source of ocean water. Together with orbital modeling, these measurements
suggested instead that asteroids with composition similar to that of CI meteoroids were the main
water source. As part of our solar system observation programme [1], using the HIFI instrument [2]
on the Herschel Space Observatory [3], we have obtained the first measurement of the D/H ratio in a
Jupiter-Family comet (103P/Hartley 2) [4]. It turned out that 103P's D/H-ratio is consistent with
VSMOW. This result substantially expands the reservoir of Earth ocean-like water to include some
comets, and is consistent with the emerging picture of a complex dynamical evolution of the early
Solar System. We discuss the implications of these observations for the origin of water and the
evolution of its distribution in the solar system.
References:
[1] Hartogh P. et al. (2009) Planet. Space Sci. 57, 1596-1606.
[2] de Graauw T. et al. (2010) Astron. Astrophys. 518, L4.
[3] Pilbrat G. et al. (2010) Astron. Astrophys. 518, L1.
[4] Hartogh, P. et al. (2011) Nature 478, 218-220
Comparison among different lunar surface ages calculation methods
by lunar crater frequency-size distribution
LI Yan-qiu, Chen Sheng-bo, Lian Yi, Guo Peng-ju
College of Geoexploration Science and Technology,
Jilin University, Changchun 130026
Abstract：Crater size–frequency distribution is a powerful method for estimating the age of a planet's
surface. According to the diameter range of craters, three chronology functional expressions are
available for calculating the geologic age of stratigraphic units, including Melosh and Vickery 1989
(﹥4km craters), Neukum 1983(﹥1km craters), and LI Kun et al 2012(﹤1km craters). Using the
LROC data of LRO are used to calculate the crater numbers owing to its high spatial resolution(0.5m
/pixel). Thus, a crater numbering criteria and new chronology functional expressions are built by the
real isotope ages surrounding Apollo 12, Apollo14, and Apollo16 landing sites areas. By comparion,
it shows that the algorithm with larger than 1km craters by Neukum 1983, performs better than the
others.
Key words: LROC ; the geologic age ; chronology functional; crater diameter
Theoretical prediction and observation evidences on the northward
drift and annual oscillation of the Earth’s core from space geodesy
Yuri Barkin 1, Shuanggen Jin
2, WenBin Shen
3
1 Sternberg Astronomical Institute at Moscow State University, Moscow, Russia
2 Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China
3 School of Geodesy and Geomatics/Key Laboratory of Geospace Environment and Geodesy of Ministry of
Education, Wuhan University, Wuhan 430079, China;
Abstarct: In the last decades, the contrast changes on of the Northern and Southern Hemispheres’
shapes have been investigated using the space geodetic observations, e.g., the secular and annual
variations of the volumes, lengths of the circles of latitude and mean radius of the Northern and
Southern hemispheres on the basis of current space geodetic data. It has shown the clear secular
trend of the center of Earth’s mass, whose mechanism was as a consequence of the secular northward
drift of the Earth’s core relative to the mantle. In this paper, the geodetic results on the secular drift
and annual oscillation of the core relatively to the mantle in the Earth’s hemispheres are reviewed
and presented. Some theoretical assumptions and phenomena are also confirmed as well as the
legitimacy and universality of the developed geodynamic model of forced oscillations of the Earth’s
core – mantle system (Barkin, 2002). For example, global DORIS observations showed the existence
of the secular polar northward drift of the center of Earths’ mass at 5.2 mm/y. This drift reflects the
Earth’s core drift at a rate of 27.4±0.8 mm/y (Barkin, 2005), i.e., the drift of the center of the core’s
mass relative to the center of the mantle’s mass. The gravitational effect of the shifting core causes
deformations of all layers of the mantle and various offsets. As a result, the mean radius of the
northern hemisphere increases with the small velocity about 0.01 mm/y, and the mean radius of the
southern hemisphere on the contrary decreases with the same magnitude of velocity - 0.01 mm/y.
This It is effect is very difficult for confirmation on the base of satellite observations. Shen et al.
(2012) also obtained related results with 0.46 ± -0.01 mm/y and -0.19 ± -0.01 mm/y for northern and
southern hemispheres respectively from global geodetic observations at 845 stations, respectively.
The theoretical value of the largest secular velocity of lengthening of latitudinal circles in the
southern hemisphere at latitude 45°S is 5.47 ±-0.12 mm/y, and in the northern hemisphere the secular
velocity of shortening of latitudinal circle (for latitude 45°N) is - 5.47±-0.12 mm/y, which are
consistent with recent results at secular velocity in 4.5 mm/y and 9.5 mm/y for the northern and
southern hemispheres (Barkin and Jin, 2006 and 2007). These geodetic observations results give a
good explanation. The asymmetric real changes in the Earth’s shape are apparently related to the
formation of the rifting and subduction zones in their asymmetrical arrangement in relation to the
Northern and Southern hemispheres.
In this paper, we study the effect of the annual planetary geodesic polar oscillations of the core,
which corresponds to a unidirectional oscillation of the center of mass of the Earth with an amplitude
of 21.3 ± 0.9 mm, and the initial phase of 35.8 ± 3.6º (Kaftan, 2004). The study of solution of the
elasticity problem of deformation of the mantle at the annual oscillation of the core of the Earth has
identified the following annual geodetic phenomenon: the annual variation of the lengths of
latitudinal circles, depending on the latitude and time t by the law -22.030cos (360º t - 35.8º) sin2Ф
mm of annual variation of the radial displacements of points on the surface of the mantle of the law
0.133cos (360º t - 35.8º) sinФ mm annual meridian points on the surface of the Earth vibrations
7.145cos (360º t - 35.8º) cosФ mm [I can’t understand this long sentence, which might be more
precisely and clearly written?]. In this report we discuss prospects of geodetic determination of these
effects with the annual period on the basis of current space-geodetic data of space geodesy.
Empirical density model of marine sediments
Robert Tenzer, Vladislav Gladkikh, Yuan Cui
Institute of Geodesy and Geophysics, School of Geodesy and Geomatics, Wuhan University, 129 Luoyu Road,
Wuhan, China
Abstract: In the context of gravimetric studies investigating the oceanic lithosphere structure and its
evolution, the sediment stripping gravity correction has been often calculated utilizing a uniform
density distribution, irrespective of physical properties and mineral composition of marine sediments.
To improve interpretation quality, some authors developed more complex density-depth equations
suitable in regional studies, where drilling and seismic data provide enough information on the
structural composition of marine sediments. Nonetheless, the empirical density model derived based
on the analysis of global datasets is not yet available. For this purpose, we analyze density samples
of marine sediments, provided by the National Geophysical Data Center (NGDC) of the U.S.
National Oceanic and Atmospheric Administration (NOAA) collected within the frameworks of the
Ocean Drilling Program (ODP) and the Deep Sea Drilling Project (DSDP). These data are used to
assess the sediment density change due to the sediment thickness and the ocean-floor depth. We
demonstrate that the density distribution exhibits a distinctive trend of the increasing density with the
sediment thickness due to the compaction and lithification. We also argue that a prevailing pattern of
the decreasing density with the increasing ocean-floor depth detected within of the upper
stratigraphic sediment sequences is likely governed by the physical properties of marine sediments
(such as its origin, transportation distance, porosity, grain size, and deposit environment). We
develop and present various empirical density models, and discussed their possible applications in
the gravimetric forward and inverse modeling of marine sediments. The analysis of NGDC dataset
reveals that the sediment density distribution can be approximated by simple functional models with
average errors better than 10%.
Keywords: compaction, density, ocean-floor spreading, marine sediments
An optical experiment to measure a torque acted by the Moon on the
Earth equator
Sahnggi Park
Electronics and Telecommunications Research Institute (ETRI),
218 Gajong-Ro Yusong-Gu Daejon South Korea, 305-700,
Abstract: The Earth acts a tidal force on the Moon to rotate the Moon synchronously, where the tidal
force induce a torque to make a synchronous spin of the Moon with the orbital motion. There should
be a reaction torque on the Earth, of which magnitude and direction are the same as them of the
torque, which is analogous to Newton's third law in the linear motion.
As considering the magnitude and the direction of the reaction torque, it is expected that the reaction
torque would be an important factor for a lot of Earth activities, flow of sea water, tides, air flows,
volcanoes, earthquakes, etc. An optical experiment to measure the reaction torque is discussed. For
the libration of the Moon facing 58% of its surface to the Earth, the largest shift of 1 m pendulum at
the equator is calculated to be 0.3043nm which can be magnified to 152.2 m by 5 km laser beam
and 5 m pendulum. The force in the reaction torque has a ratio, a/g, with the gravitational force at the
Earth equator surface,
a/g = [r2m2(2Gm1Rm/d3)sin]/[r1m1(Gm1/Re
2)]
d sin=Rmsin7.
The ratio, a/g, is calculated as 1.522╳10-10
to give a 0.3043 nm shift with 1 m pendulum for 58 % of
Moon face. Figure shows a possible experiment to measure 0.3043 nm shift. A pendulum of 5 m
length and a laser beam with multiple reflection mirrors are set on an optical table. The total path
length of laser beam is 5 km. A monitor displays a shift of laser beam magnified to 152.2 m. The
whole system is enclosed by a chamber to block air flow.
5 m pendulum
monitor
laser
5 cm
mirror
5 m pendulum
monitor
laser
5 cm
mirror
Gravimetric forward and inverse modeling methods for global
recovery of the crustal density structures and crust-mantle interface
Robert Tenzer, Wenjin Chen
Institute of Geodesy and Geophysics, School of Geodesy and Geomatics, Wuhan University, 129 Luoyu Road,
Wuhan, China
Abstract: The gravimetric inverse problem for finding the crust-mantle (Moho) density contrast is
formulated in this study based on the assumption that the crust density structures and the crust
thickness are a priori known, for instance, from results of seismic studies. The functional relation
between the refined gravity data and the Moho density contrast is defined by means of the Fredholm
integral equation of the first kind. The refined gravity data used for solving the gravimetric inverse
problem should (optimally) comprise only the gravity signal attributed to the Moho geometry. This
assumption is still restricted by the limited knowledge about the density structures within the
lithosphere and sub-lithosphere mantle. The expressions for computing the refined gravity data and
the Moho density contrast are defined in spectral domain utilizing various spherical functions, which
describe globally the crustal density structures and the Moho density interface. The functional model
is formed for the density contrast defined relative to the adopted homogenous crustal density model.
A more refined formulation of the inverse problem is also given using additional constraining
parameters. These parameters are based on empirical models, which describe theoretical spatial
variations of the Moho density contrast. In particular, the density changes due to the mantle
convection (i.e. ocean-floor spreading) are utilized within the oceanic lithosphere, while the
depth-dependent density model is adopted within the continental lithosphere.
Keywords: crust, forward modeling, gravimetric inverse problem, Moho interface
Signature of the ocean-floor spreading, hot spots, and subducted
slabs in marine gravity data
Robert Tenzer, Wenjin Chen
Institute of Geodesy and Geophysics, School of Geodesy and Geomatics, Wuhan University, 129 Luoyu Road,
Wuhan, China
Abstract: Evidence of the ocean-floor spreading was given from marine magnetic surveys and later
independently verified from the age dating of ocean-floor rock samples and from seismic studies.
The process of oceanic lithosphere cooling directly controls the lateral density distribution across
ocean-floor profiles. The increasing lithospheric density with age should be detectable in marine
gravity data. This is demonstrated using refined gravity data, which are corrected for gravitational
signals of the anomalous crustal density structures and the Moho geometry. The additional correction
term for the lithospheric thermal cooling reveals inhomogeneous lithosphere structures such as hot
spots and subducted oceanic slabs.
Keywords: density, gravity, ocean-floor spreading, oceanic lithosphere, spreading ridge axes,
subduction
Vestan lithologies mapped by the Visual and Infrared Spectrometer
on Dawn
E. AMMANNITO1, M.C. DE SANCTIS
1, F. CAPACCIONI
1, M.T. CAPRIA
1, J.P. COMBE
2, S.FONTE
1, A.
FRIGERI1, S.P. JOY
3, A. LONGOBARDO
1, G. MAGNI
1, S. MARCHI
4, T.B. MCCORD
2, L.A. MCFADDEN
5,
H.Y. MCSWEEN6, E. PALOMBA
1, C.M. PIETERS
7, C.A. POLANSKEY
8, C.A. RAYMOND
8, J.M. SUNSHINE
9,
F. TOSI1, F. ZAMBON
1, C.T. RUSSELL
3
1 Istituto di Astrofisica e Planetologia Spaziali, INAF, Rome, Italy
2 Bear Fight Institute, 22 Fiddler’s Road, Box 667, Winthrop, Washington 98862, USA
3 Institute of Geophysics and Planetary Physics, University of California, Los Angeles, California 90095-1567,
USA 4 NASA Lunar Science Institute, Southwest Research Institute, 1050 Walnut St, Suite 300, Boulder, CO 80302, USA
5 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
6 Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996-1410, USA
7 Brown University, Department of Geological Sciences, Providence, RI 02912, USA
8 Jet Propulsion Laboratory, Pasadena, California 91109, USA
9 University of Maryland at College Park, MD 20742-2421, USA
Abstract: 4 Vesta is known to have a surface of basaltic material through visible/near-infrared
reflectance spectroscopy. Vesta’s spectrum has strong absorption features centered near 0.9 and 1.9
μm, indicative of Fe-bearing pyroxenes. The spectra of HED (howardite, eucrite and diogenite)
meteorites have similar features. This led to the hypothesis that Vesta was the parent body of the
HED clan and the discovery of a dynamical Vesta family of asteroids (Vestoids) provides a further
link between Vesta and HEDs. Data from the Dawn VIR (Visible InfraRed mapping Spectrometer)
characterize and map the mineral distribution on Vesta, strengthen the Vesta – HED linkage and
provide new insights into Vesta’s formation and evolution. In this work we present global lithological
maps of the Vestan surface based on VIR acquisitions with a spatial sampling of 200 m. The
lithological maps are based on the distribution of the spectral positions of pyroxene absorption bands
in the 0.7 - 2.5 μm range. With respect to the previous versions of the same maps, the spatial
sampling has been improved and the explored region has been extended towards northern latitudes
up to +65 deg. The maps presented here confirm the results obtained with the dataset acquired by
VIR with a spatial sampling of 700 m. The maps also partially agree with the ground and HST based
observations: they confirm the background surface being an assemblage of howardite or polymict
eucrite, the location of a diogenitic-rich spot; however, there is no evidence of extended olivine-rich
regions in the equatorial latitudes. Exposed diogenite is revealed by VIR on the Rheasilvia basin
floor, indicating that material of the lower crust/mantle was exposed; however, VIR also detected
diogenites elsewhere. The diogenite distribution is fully consistent with petrological constraints, but
does not provide unambiguous constraints for the proposed formation models. The maps presented
here favor the hypothesis of magma ocean models.
ANOMALIES OF DENSITY, STRESSES, AND GRAVITY IN THE
INTERIOR OF EARTH AND MARS AND POSSIBLE
GEODINAMICAL CONSEQUENCES: A COMPARATIVE
ANALYSIS
N. A. Chujkova, L.N. Nasonova, T.G. Maximova
Moscow M V Lomonosov State University, Sternberg Astronomical Institute, Moscow, Russia
Abstract: Formulas that include in the quadratic approximation the contribution of anomalous masses,
distributed in height to the reference ellipsoid, to the Stokes constant have been derived. It is shown
that the contribution of the quadratic terms is especially important in the case of dipole (by height)
distribution of anomalous masses and it is compared in order of magnitude to the linear contribution.
For Mars, the contribution of the quadratic terms is especially great , because its range of variations
in relative heights of the relief is greater by an order of magnitude than that for the Earth. The
method of determining the depths of compensation for topography harmonics of various degrees and
orders is developed. Based on analysis of the depth distribution compensation histograms the most
probable levels of compensation for topographic inhomogeneity are determined. It is shown that the
isostatic compensation of the relief of the Earth and Mars is in the depth range 0-1400 km. It is
shown that the depths of the basic compensation levels for the Earth are in good agreement with the
seismic data.
For selected levels the maps of the lateral distributions of compensating masses are
constructed.We show that these abnormal structures force the abnormalities of internal gravitational
field, which may cause the convective motions to appear in the mantle and the core of the planet,
responsible for the existence of the Earth's magnetic field and the lack thereof for Mars.
The possible isostatic unaligned vertical stresses in the crust and mantle of the Earth and Mars
are calculated. The resulting distribution of vertical compressive and tensile stresses are well
correlated with the distribution maps for the earth quakes and volcanic craters of enhanced density
for Mars. For Mars, the maximum stress values much higher than earthly values, indicating greater
strength of Martian lithosphere .
Keywords: Earth, Mars, gravity, isostatic compensation, internal structure, crust, mantle, core,
plumes, convection, stresses
Automatic recognition of impact craters on Mars based on DEM
data
Tengyu Zhang 1,2
, Shuanggen Jin1
1 Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China
2 University of Chinese Academy of Sciences, Beijing 100049, China
Abstract: The recognition of impact craters can provide information on impact history and Martian
evolution process as well as for Martian rover landing. Most previous studies about machine
detection of impact craters on Mars are based on imagery data, however, it has large uncertainty in
image processing. In this study, we present a novel approach for automatic recognition of impact
craters based on digital topography data from High Resolution Stereo Camera on Mars Express.
More small size craters are detected by utilizing the high resolution DEM data. Topographic
curvature, which delineates impact crater on DEM, can be deduced from topography data. The
thresholding map of curvature is transformed into a binary map, from which we can detect impact
craters by combination of segmentation and flooding algorithms. The more impact craters on Mars
with confirmation algorithm can be effectively distinguished truly, which are added the existing
catalog of manually identified Martian craters.
Exploration of the Galilean Satellites: The Ganymede Laser
Altimeter (GALA) on -board the JUICE Mission
Hauke Hussmann
DLR Institute of Planetary Research, Rutherfordstr. 2, 12489 Berlin, Germany
Abstract: In 2012 ESA has selected the Jupiter Icy Moons Explorer (JUICE) as the next L-class
mission in the Cosmic Vision program. Besides Jupiter and its magnetosphere, the Galilean Satellites
are major targets of this mission. Europa and Callisto will be investigated by flybys while the
spacecraft is in Jupiter orbit. Finally, the JUICE spacecraft will go into orbit around Ganymede. It
will be the first orbiter around a moon in the outer solar system. First JUICE will be in a highly
elliptical orbit mainly to investigate Ganymede’s magnetosphere and to perform distant remote
sensing. The final mission phases will be 500 and 200 km altitude polar orbits for targeted
observations, altimetry and gravity field determination . The JUICE launch is scheduled for
mid-2022. Arrival at Jupiter will be in 2030 followed by a three- years mission phase in the Jupiter
system.
The Ganymede Laser Altimeter (GALA) has been selected by ESA for the Jupiter Icy Moons
Explorer (JUICE) mission payload. GALA will focus on geodetic and geophysical investigations of
the icy satellites Europa, Ganymede and Callisto. Here, we describe the scientific objectives, its
expected performance, and the status of the instrument development.
Case for Future Exploration of Venus
Sanjay S. Limaye
Space Science and Engineering Center University of Wisconsin, Madison, Wisconsin, USA
Abstract: We have learned a lot about Venus in the first fifty years of space exploration than we ever
new before then. After the practice and survey missions of Mariner 2 followed by Venera and other
missions, the recent extended observations from Venus Express add to the many puzzles presented
by Magellan, Pioneer Venus and the VeGa balloon missions about Venus – why does Venus spin so
slowly and backwards? When did Venus lose its surface water? Why did Venus lose its water? Did
life ever evolve on Venus? Why does not Venus have a magnetic field? Why does the atmosphere of
Venus move faster than the planet? Is Venus slowing down or spinning up? Why does the sulfur
dioxide abundance above the clouds show large variations over time and location on Venus? Does
Venus have active volcanoes now? How does Venus lose its heat? Are there lessons for Earth
regarding its future climates? These are just a few of the key questions that still need answers and
hence new observations from capable space missions and ground based or earth-orbiting telescopes.
The observations required need a mix of orbiters, entry probes, longer life landers and floating
platforms at multiple levels. Some investment in developing high temperature
electronics/communications and operations of instruments is needed. Learning more about the
surface of Venus, its detailed gravity field, interior and its thick atmosphere will require many
different approaches for instruments coverage a large electromagnetic spectral range. However,
such an observation campaign is an ambitious effort. With limited budgets and more exploration
targets, the resources available for Venus to most space faring nations are limited and it is only
through collaboration and coordination of international efforts that this may be feasible.
Accomplishing this goal is worthy and useful and possible in the next decade and beyond.
Structure and Escape of Extrasolar Planet Upper Atmospheres
R. V. Yelle and T. Koskinen
Lunar and Planetary Laboratory, University of Arizona
Abstract: The atmospheres of extra-solar planets are small orbital distances are subject to intense UV
radiation from their primary stars. Absorption of this radiation heat the atmosphere to high
temperatures, alters the composition of the atmosphere from molecular species to atomic and ionic
species and drives escape of the atmosphere. The high temperatures and low molecular weight
cause greatly extended upper atmospheres that can be detected and studied in UV transit
observations. The rapid escape of H and H+ drags along heavier species such as O+ and Si++, that
can also be observed in transit measurements. This talk will briefly review the basic theory for these
highly-irradiated planets, present some recent results on models for extra-solar upper atmospheres,
and discuss the implications of upper atmosphere observations for the structure of the lower
atmospheres of extra solar planets.
Planetary Geodesy from Precision Spacecraft Tracking
Luciano Iess
Sapienza Università di Roma
Abstract: In the context of planetary exploration, with the broad term “radio science” one indicates a
technique exploiting radio links between a ground antenna and a deep space probe to carry out
scientific investigations in planetary geodesy, solar system dynamics, fundamental physics and
atmospheric science. On most space missions radio science experiments shared the same
instrumentation used in spacecraft tracking and navigation, but the need for increased accuracies in
radio-metric measurements, driven by planetary geodesy and fundamental physics investigations, led
to the development of dedicated transponders and ground systems. A Ka-band radio system (32-34
GHz) was used on the mission Cassini to carry out the most accurate test of general relativity to date
and to determine the gravity fields of the Saturnian satellites, including the tidal deformations of
Titan. The gravity fields of Jupiter, Mercury and the Galilean moons will also be measured with
much increased accuracy by means of precise Doppler tracking of the spacecraft Juno (NASA),
BepiColombo and JUICE (ESA). All these missions are endowed with microwave systems providing
range rate measurement accuracies of about 1 micron/s over time scales of 1000 s. This seminar
reviews the methods of precision spacecraft tracking and their application to planetary geodesy, with
examples from past and ongoing missions. We will outline also the novel opportunities offered by
interferometric measurements to network of landers on Mars and the Moon for ultra-precise
measurements of rotation and tides.
Predicting the mean motion resonance formation in the Kepler
observed systems
Su Wang
Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China
Abstract: The Kepler Mission has released more than 2321 transiting planet candidates. There are
about 85 candidate systems with three planets. Among them, eight systems are potentially in 4:2:1
MMRs, and five systems are possibly in 3:2:1 MMRs. In this paper, we study the formation of mean
motion resonance systems focusing on the influence of stellar accretion rate, stellar magnetic field
and the speed of migration. We generate 224 runs assuming a system with a solar-like star and three
planets around. From the statistic results, we find that high magnetic field and the star accretion rate
larger than 10-8
M☉yr-1
or smallerthan 5×10-9
M☉yr-1
are propitious to the formation of 2:1 and 3:2
MMRs. The speed reduction factor of type I migration f1=[0.1, 0.3] facilitates the formation of 2:1
MMR, while f1≥0.3 facilitates the formation of 3:2 MMR. Under such formation scenario in three
planets system, 2:1 MMR can be formed in a high probability, while 3:2 MMR is difficult to form
especially the 3:2:1 MMRs. If there is extra planet in the inner region or the outer region of the three
planets system, 3:2:1 MMRs can be formed and the original 4:2:1 MMRs are not affected by the
extra planets. Thus, it is possible that there are extra planets survived in the three planets systems
observed by Kepler.
A method of Image Matching Based on Lunar Image
HE YU, XU QING, LAN CHAOZHEN
Institute of Surveying and Mapping, Zhengzhou,China
Abstract: Application of satellite, manned space and deep space exploration is three important
application field in the aerospace technology, deep space exploration of our country is the inevitable
selection based on the achievement in the first two areas. The lunar is the nearest bodies from the
earth in the solar system, is a natural satellite of the earth.So all the countries in the world look lunar
detection as a starting point and focus in the space program and the lunar exploration is the
beginning in human space exploration.
In 2007 October, China's lunar exploration satellite "Chang'e-1 " launched successfully, it marked
that China 's lunar exploration project had begun, the lunar surveying and mapping was a very
important scientific goals by using the exploration data. This goal need to make lunar digital terrain
map, the lunar digital elevation model (DEM ) and the lunar digital orthophoto map ( DOM ), and
make the lunar 3-D image. To achieve this goal, Chang'e-1 satellite carried three line array CCD
stereo camera to obtain images of lunar surface, and a laser altimeter to get the lunar surface height
data.
In order to make full use of Chang'e-1 lunar exploration data, and combined with the lunar
exploration science objectives, to improve China's lunar scientific knowledge and research ability,
using CCD image data and laser altimetry data to do the photogrammetry has important significance.
This paper mainly discussed the image matching method which is the key of DEM generation using
CCD images and laser altimetry data.
Because the moon image feature is poor, the matching precision will lose in iamge matching, so
multiple constraints will consider in image matching. In this paper the corresponding points were
acquired by the method as: first Wallis filtering was used to increase image contrast, then SURF
operator was used to extract feature points, and then from coarse to fine image matching method to
acquire image corresponding points.
At last we used the actual date acquired by Chang'e-1 to validate the algorithm. The result shows this
algorithm can extract the corresponding points effectively, and the number of these points can
generate DEM better.
Tidal evolution of the Kepler-10 system
DONG Yao, JI Jianghui
Purple Mountain Observatory, Chinese Academy of Sciences
Abstract: We investigate by N-body numerical methods the tidal evolution of the Kepler-10 system,
which consists of an inner rocky planet and an outer terrestrial planet, by considering various initial
eccentricity pairs that follow conservation of angular momentum of the system. Our results cover the
range of all reasonable initial eccentricities with various mass ratios of the two planets for the
Kepler-10 system, all initial eccentricity pairs can produce the present observed orbits within certain
errors. Moreover, we propose a possible planetary formation scenario for the Kepler-10 system: both
planets may form from a distant region in the disc, then the inner planet may experience
planet–planet scattering, following as tidal decay and circulation. However, the outer companion
may undergo mainly disc migration, judging from our model. Finally, we discuss the future work to
investigate the coupling interaction of tide and gravitation in the Kepler candidate multi-planet
systems, on the basis of numerical simulations and theoretical analysis.
Interaction of Solar Wind with the Moon: A New View from the
SARA/Chandrayaan-1
Anil Bhardwaj1, M.B. Dhanya
1, Abhinaw Alok
1, Satheesh Thampi
1, Stas Barabash
2,
Yoshifum Futaana2, Martin Wieser
2, Peter Wurz
3, Audrey Vorburger
3, Mats Holmström
2,
Charles Lue2, Kazushi Asamura
4, Shahab Fatemi
2
1 Space Physics Laboratory, Vikram Sarabhai Space Centre, Trivandrum, India
2 Swedish Institute of Space Physics, Kiruna, Sweden
3 University of Bern, Switzerland
4 Japan Aerospace Exploration Agency, Japan
Corresponding author: [email protected]
Abstract: The Sub-keV Atom Reflecting Analyzer(SARA) experiment aboard the first Indian
lunar mission Chandrayaan-1 consisted of two sensors mounted at 90 degree to each other on the
top deck. While the Chandrayaan Energetic Neutrals Analyzer (CENA) measured energetic neutral
atoms (ENAs) in the 0.1-3keV energy range, the Solar Wind Monitor (SWIM) measured ions in
the same energy range in lunar environment. The observations made by the SARA have revealed
several new and interesting aspects about the solar wind interaction with the Moon, which include:
(1) substantial (0.16 ± 0.05) and sustained back-scattering of solar wind protons incident on the lunar
surface as neutral hydrogen atoms (hydrogen ENAs); (2) discovery of mini-magnetosphere on Moon
using back-scattered hydrogen ENAs; (3) preferential back-scattering of solar wind ENAs in
the sunward direction; (4) finding that the Maxwell-Boltzmann distribution fits the back-scattered
ENAs energy spectrum, thus deriving the characteristic temperature for ENAs of 60-140 eV; (5) a
linear correlation between solar wind bulk velocity and the temperature of back-scattered
ENAs; (6) first global ENA map covering 89% of the lunar surface, which correlate well with the
magnetic field map; (7) huge (~50%) deflection of solar wind protons around strong magnetic
anomalies; (8) accelerated pick-up ions in lunar environment; (9) small (<~1%) scattering of solar
wind protons from lunar surface; (10) detection of ions in the near-lunar plasma wake (night side)
under varying interplanetary magnetic field conditions; and (11) presence of large (+135 V)
electric potential over lunar magnetized regions.
These results have questioned our earlier understanding that the solar wind is completely absorbed
on the lunar surface, and imply that the physics of plasma-regolith interaction is complex and
needs to be understood. They also imply that solar wind interaction with magnetic anomaly regions
on Moon is quite different. The SARA observations suggest that similar processes may happen on
other atmosphere-less bodies covered with regolith in the solar system as well as in extra-solar
system.
Variations and effects of the Venusian Bow Shock from VEX mission
Yansong Xue and Shuanggen Jin
Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China.
Email: [email protected]; [email protected]
Abstract: The upper atmosphere of Venus is not shielded by planetary magnetic field from direct
interaction with the solar wind. The interaction of shocked solar wind and the ionosphere results in
ionopause. Magnetic barrier, the inner region of dayside magnetosheath with the dominated magnetic
pressure effects the solar wind instead of the ionopause at solar maximum. Therefore, the structure
and interaction of venusian ionosphere is very complex. Although the recent Venus Express (VEX)
arrived at Venus in April 2006 provides more knowledge on the Venusian ionosphere and plasma
environment, compared to Pioneer Venus Orbiter (PVO) with about 14 years of observations, but
some important details are still unknown, e.g., long Venusian bow shock variations and e®ects. In
this paper, the bow shock positions of Venus are determined and analyzed from magnetometer (MAG)
and ASPERA-4 of the Venus Express mission from May 28, 2006 to August 17, 2010. Results show
that the altitude of BS was mainly a®ected by SZA (solar zenith angle) and Venus bow shocks
inbound and outbound are asymmetry.
Keywords: Venus, Bow shock, Magnetic field, Venus Express.
A refined gravity field model of Venus VGM2013 using high resolution
topography data
Yan Jian-Guo1 Xu Lu-Yuan
2, Li Fei
1,2
1 The State Key Laboratory of Information Engineering in Surveying, Mapping and Remote Sensing, Wuhan
University, Wuhan 430079, China 2 Chinese Antarctic Center of Surveying and Mapping(CACSM), Wuhan University, Wuhan 430079, China
Abstract: High resolution gravity field is significantly important for Venus exploration. In this paper,
we referred to the method of gravity field refinement on the Earth, Moon and Mars and gave a new
3-dimensional Venus gravity field VGM2013 by using the latest topography and gravity model,
residual terrain model (RTM) and the Airy-Heiskanen isostatic compensation model. We found the
optimal global compensation depth of Venus is about 30km, and the crust density may be less than
2700-2900 kg/m3, which is generally recognized now. The VGM2013 is the first 10 km-magnitude
Venus gravity field till now, and the ultimate results are the 3-dimensional surface gravity
acceleration and gravity disturbances. This results are beneficial for Venus spacecraft’s orbit
determination and landing navigation, and can be used as a priori model for Venus gravity field
simulation and inversion studies. Given that VGM2013 does not incorporate gravity field
observations beyond degree 120, it’s not recommended for direct geological and smaller-scale
geophysical interpretation.
Keywords: Venus, gravity field refinement, residual terrain model (RTM), isostatic compensation,
VGM2013
Analysis of Epipolar Line for Mars Express HRSC Linear Pushbroom
Imagery
Xun Geng
Institute. Surveying and Mapping,China
Abstract: The epipolar line is essential for aero-triangulation, feature extraction and automatic DEM
extraction. After epipolar resampling, the conjugate points are located along the same row. Because
of the complex image geometry of linear pushbroom imagery, the epipoar line of linear pushbroom
imagery is not straight line. In this paper, the epipolar geometry of Mars Express HRSC is analyzed
based on projection trajectory. Experiment result demonstrates that the epipolar line of HRSC image
is hyperbola line, while in local area it can be replaced by line.
Keyword: Mars; Mars Express; HRSC; Linear Pushbroom Imagery; Epipolar Image;
The forced and free physical libration of the Moon with ellipsoidal
liquid core and elastic mantle
Y. Barkin1, H. Hanada
2, J. Ferrandiz
3, K. Matsumato
2, S. Sasaki
2, M. Barkin
4
1 Sternberg Astronomical Institute, Moscow, Russia.
2 National Astronomical Observatory of Japan, Mizusawa, Japan;
3 Alicante University, Alicante, Spain;
4 Moscow Aviation Institute, Moscow, Russia.
E-mail: [email protected];
1. Analytical theory. The main study here is a construction and development of a highly accurate
analytical theory of physical libration of the two-layer Moon (with uniform ellipsoidal liquid core
and non-spherical elastic mantle). In this theory the physical libration of the Moon, regarded as a
system of interacting core and mantle, in the gravitational field of the Earth and other celestial bodies
has been developed. The core of the Moon is modeled by ellipsoid with an ideal homogeneous fluid.
The mantle is considered as non-spherical elastic body. The theory is developed on the basis of the
canonical equations in Andover - Poincare variables and by special methods of the perturbation
theory on construction of quasi-periodic solutions and investigation of their vicinity (based on the
relevant equations in variations). The tables of values of the amplitudes and periods of forced and
free librations for Andoyer – Poincare’s variables describing the libration of the Moon and the core,
for the variations of the components of the angular velocity of rotation of the Moon and the angular
velocity of rotation of the coordinate system of Poincare (with respect to which a simple fluid motion
is determined) have been obtained and studied. In constructing of the libration theory of the Moon
the precision lunar orbit has been accepted. In first we have studied contributions in librations of the
Moon of the second harmonic of selenopotential in accordance with the modern Selena model of
gravitational field of the Moon (Matsumoto et al., 2010). The novelty of the theory and its practical
significance are determined by the following principal provisions: 1. New forms of equations of
physical libration of the two-layer model of the Moon (in particular in Andoyer – Poincare variables)
and new methods for their study; 2. Highly accurate description of the developments of spherical
functions of the coordinates of the Moon, in the expression of the force function; 3. The new
two-layer Mizusawa’s model of the Moon and Selena’s model of the gravitational field of the Moon;
4. Cassini’s rotation of the Moon, forced and free librations of the Moon in analytical form and their
tables; 5. Dynamical effects in forced and in free librations caused by a liquid core; 6. Dynamical
effects in forced and free librations of the Moon caused by its elasticity; 7. Determination of the forth
mode of free libration caused by the liquid core; 8. Identification of some terms of modern
Rambaux-Williams’s empirical theory. New important terms in physical libration in longitude were
discovered. In particular the big term (with amplitude 211”) but with very long period 67049
days (183.6 yr).
2. Determination of the period, amplitude and phase of the fourth mode of the free libration of
the Moon. We have been compare free libration terms from our analytical theory with some
unidentified terms from empirical theory (Rambaux, Williams, 2011). In results 8 unidentified terms
for classical variables in empirical theory were explained and amplitude, initial phase of the Moon
free libration have been determined. The period of free libration of the pole of the Moon with liquid
ellipsoidal core appreciated by us in 205.7 yr. The amplitude and initial phase of Poincare’s
long-periodic argument of the free libration in pole motion due to liquid core have been determined
in 0”0395 and -134 degrees (for initial epoch 2000.0 JD). In accordance with developed analytical
theory this period corresponds to the sum of dynamic compressions of the core in 7.24x10(-4), that is
in agree with seismographic data and data of laser observations (Barkin, Hanada et al., 2012). In
assumption about similarity of ellipsoidal core and the entire Moon we have obtained the estimations
of oblatenesses of the liquid core: 4.42x10(-4) and 2.83x10(-4).
Theoretical prediction and observation evidences on the northward
drift and annual oscillation of the Earth’s core from space geodesy
Yuri Barkin 1, Shuanggen Jin
2, WenBin Shen
3
1 Sternberg Astronomical Institute at Moscow State University, Moscow, Russia
2 Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China
3 School of Geodesy and Geomatics/Key Laboratory of Geospace Environment and Geodesy of Ministry of
Education, Wuhan University, Wuhan 430079, China;
Abstract: In the last decades, the contrast changes of the Northern and Southern Hemispheres’
shapes have been investigated using the space geodetic observations, e.g., the secular and annual
variations of the volumes, lengths of the circles of latitude and mean radius of the Northern and
Southern hemispheres on the basis of current space geodetic data. It has shown the clear secular
trend of the center of Earth’s mass, whose mechanism was as a consequence of the secular northward
drift of the Earth’s core relative to the mantle. In this paper, the geodetic results on the secular drift
and annual oscillation of the core relatively to the mantle in the Earth’s hemispheres are reviewed
and presented. Some theoretical assumptions and phenomena are also confirmed as well as the
legitimacy and universality of the developed geodynamic model of forced oscillations of the Earth’s
core – mantle system (Barkin, 2002). For example, global DORIS observations showed the existence
of the secular polar northward drift of the center of Earths’ mass at 5.2 mm/y. This drift reflects the
Earth’s core drift at a rate of 27.4±0.8 mm/y (Barkin, 2005), i.e., the drift of the center of the core’s
mass relative to the center of the mantle’s mass. The gravitational effect of the shifting core causes
deformations of all layers of the mantle and various offsets. As a result, the mean radius of the
northern hemisphere increases with the small velocity about 0.01 mm/y, and the mean radius of the
southern hemisphere on the contrary decreases with the same magnitude of velocity - 0.01 mm/y.
This effect is very difficult for confirmation on the base of satellite observations. Shen et al. (2012)
also obtained related results with 0.46 ± -0.01 mm/y and -0.19 ± -0.01 mm/y for northern and
southern hemispheres respectively from global geodetic observations at 845 stations. The theoretical
value of the largest secular velocity of lengthening of latitudinal circles in the southern hemisphere at
latitude 45°S is 5.47 ±-0.12 mm/y, and in the northern hemisphere the secular velocity of
shortening of latitudinal circle (for latitude 45°N) is - 5.47±-0.12 mm/y, which are consistent with
recent results at secular velocity in 4.5 mm/y and 9.5 mm/y for the northern and southern
hemispheres (Barkin and Jin, 2006 and 2007). These geodetic observations results give a good
explanation. The asymmetric real changes in the Earth’s shape are apparently related to the formation
of the rifting and subduction zones in their asymmetrical arrangement in relation to the Northern and
Southern hemispheres.
In this paper, we study the effect of the annual planetary geodesic polar oscillations of the core,
which corresponds to a unidirectional oscillation of the center of mass of the Earth with an amplitude
of 21.3 ± 0.9 mm, and the initial phase of 35.8 ± 3.6º (Kaftan, 2004). The study of solution of the
elasticity problem of deformation of the mantle at the annual oscillation of the core of the Earth let us
to identify and describe the set new geodetic phenomena. From them the annual variation of the
lengths of latitudinal circles, depending on the latitude and time t by the law -22.030cos (360º t -
35.8º) sin2Ф mm. The annual variation of the radial displacements of points on the surface of the
mantle of the law 0.133cos (360º t - 35.8º) sinФ mm. And the annual meridian displacements of the
points on the surface of the Earth by the law 7.145cos (360º t - 35.8º) cosФ mm. In this report we
discuss prospects of geodetic determination of these effects with the annual period on the basis of
current space-geodetic data.
Unified theory of planetary processes of planets, satellites and the Sun
Yuri Barkin
Sternberg Astronomical Institute at Moscow State University, Moscow, Russia [email protected]
Abstract: The key issue of the theory of natural planetary processes on the Earth and other celestial
bodies, is the question about the sources of endogenous activity and the underlying mechanism of
energetic excitation of celestial bodies. We offer a solution to this difficult question on the basis of
the mechanism of excitation of the shells of a celestial body by gravitational attraction of the external
celestial bodies. The main provision of the developed geodynamic concept lies in the fact that the
planets, moons and the sun are the define system of shells (of the core, the mantle, and others), which
make to each other a translational-rotational motion and deformation changes under the influence of
others external celestial bodies (Barkin, 2002). We have developed the fundamentals of this
geodynamic model of the forced and free oscillations of the shells. In particular, the tides in the
visco-elastic mantle of the planet, which are generated by the gravitational forces of interaction with
the movable core. They change over time leads to the dissipation of the mechanical energy in the
material of planet, which is transformed into heat and generates the temperature field inside the
planet. As a model of the undeformed planet e consider viscoelastic homogeneous sphere, the
material behavior is described by the Kelvin - Voigt model. It is determined by the strain rate tensor
of deformations of rotating planet and the average temperature field inside the planet. The integral
heat flow as global so in the northern and southern hemispheres jf the Earth are deterined. The most
important question, of course, at all times in the history of geosciences was the question about the
source of energy (Khain, Lomize, 2005), which provides unprecedented activity of the Earth, and it
is now known that many other celestial bodies. The known energy mechanisms such as radiogenic
heat, tidal friction and others can not explain either by a total energy or cyclical processes, not to
mention the above fine planetary phenomena of inversion, step-by-step phenomena, the activity of
the polar regions and others (Barkin, 2002). The current research clearly shows that tidal friction
gives only a small contribution to the total observed heat flow of the Earth (~ 0.4 TW) across the
surface of the Earth, which is currently estimated at 46 ± 3 TW, i.e. order of one percent. The
dissipation of tidal energy on Enceladus can explain only 1 part of 27 of the observed heat flow. The
dissipation of tidal energy in the satellite Io explains only a small part of the observed heat flow and
the endogenous activity of the satellite (Barkin, 2011). All these problems are solved with the help of
the geodynamic mechanism of the forced relative oscillation of the core and mantle of the Earth
(Barkin, 1999, 2002). These displacements of the core lead to a shift of the center of mass of the
Earth relative to the mantle, which is currently available for the study of space geodetic techniques
(satellite methods). Currently, revealed a wide range of oscillations of the center of mass of the Earth
(Barkin et al., 2007; Gobinddass et al., 2009;) and discovered his secular trend towards the north (the
area of the Taimyr Peninsula) (Barkin, 1995). On the other hand, the displacements of the center of
mass of the Earth can restore the style and features of the relative displacements of the core and
mantle of the Earth, to study geodynamic consequences of these shifts, such as deformation of the
mantle, the variations of its elastic energy, power dissipation and heat flux of the planet, the other
physical fields, the redistribution fluid masses and other studies carried out effectively solve the
energy issue in the life of the planets and satellites.
In particular the power of dissipation of the elastic energy of the mantle for the observed oscillations
of the core and according to our estimates may be 1000 - 10,000 terawatt (TW). This is a huge value
of power with a vengeance explains all the endogenous activity of the Earth. Regarded geodynamic
model of the relative displacements and oscillations of the core and mantle explains all the
fundamental properties of planetary processes on Earth and other planets, satellites and Sun:
cyclicality, unity, synchronicity, inversion, polar activity, step-by-step phenomena, pilobraznost,
orderliness, twisting of layers of the mantle, the pear-shaped, versatility. All the above phenomena
and properties of endogenous activity of the celestial bodies are illustrated in report on the exaples of
natural processes on Earth, the Sun, the Moon Enceladus, Titan, Mars, etc.
GRAIL lunar gravity field recovery: simulation studies and first real
data results
Oliver Baur 1, Beate Klinger
1,2, Torsten Mayer-Gürr
2
1 Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, 8042 Graz, Austria
2 Institute of Theoretical Geodesy and Satellite Geodesy, Graz University of Technology, Steyrergasse 30/III,
8010 Graz, Austria
Abstract: The NASA mission GRAIL (Gravity Recovery and Interior Laboratory) makes use of
low-low Satellite-to-Satellite Tracking (ll-SST) between the two spacecraft GRAIL-A and GRAIL-B
to determine a high-resolution gravity field solution of the Moon. The mission concept is inherited
from the GRACE (Gravity Recovery and Climate Experiment) project, a space gravimetry mission
mapping the terrestrial gravity field. Since the Moon is in synchronous rotation with the Earth, direct
(radio) tracking of the satellites on the farside is impossible, but GRAIL provides global coverage of
inter-satellite tracking data. Furthermore, ll-SST observations are much more sensitive to
gravitational features than ground-based orbit tracking. Therefore, compared to previous missions,
GRAIL enables a more accurate estimation of the lunar gravity field, with a much higher spectral and
spatial resolution. The accurate knowledge of the lunar nearside and farside gravity is essential to
improve the understanding of the Moon’s interior structure and its thermal evolution.
We conducted a series of sensitivity studies based on simulated orbit information (positions) and
ll-SST measurements (ranges, range rates, range accelerations). Observations are simulated on the
nearside as well as on the farside (1) during the time span of the GRAIL science phase, (2) for
different orbit altitudes and varying separation distances, (3) for different orbit/ll-SST noise levels.
Furthermore, we analyzed (up to) three months of real data in order to derive a preliminary lunar
gravity field model from GRAIL ll-SST measurements. We show that the availability of global
inter-satellite tracking data improves the spatial resolution of the lunar nearside and farside
compared to previous gravity field models of the Moon. Importantly, the GRAIL mission enables the
estimation of a high-resolution gravity field model without any regularization.
Integration of Chang’E-2 Imagery and LRO Laser Altimeter Data for
Precision Lunar Topographic Modeling and Analysis
Bo Wu1, Han Hu
1,2, Jian Guo
1, Si Qiao
1, Yitao Lou
1, Meizhen Wang
1,3
1 Department of Land Surveying & Geo-Informatics, The Hong Kong Polytechnic University, Hung Hom, Kowloon,
Hong Kong 2 State Key Laboratory of Information Engineering in Surveying Mapping and Remote Sensing,
Wuhan University, China
3 School of Geographic Science, Nanjing Normal University, China
Abstract: Lunar topography is one of the principal measurements quantitatively describing the body
of the Moon. Lunar topography together with gravity data is critical to understanding the crust
structures which would have major implications for the thermal history of the Moon. High resolution
and precision lunar topographic data also play critical roles in lunar exploration missions, such as
selection of landing sites, safety maneuver of lunar vehicles or robots, and navigation of astronauts in
ground operations.
Lunar orbital imagery and laser altimeter data are two major data sources for lunar topographic
modeling. Most of the previous work has processed imagery and laser altimeter data separately.
Usually though there are inconsistencies between the topographic models derived from them. This
research presents an endeavor to integrate the cross-mission and cross-sensor data (i.e., Chang’E-2
imagery and LRO’s Lunar Orbiter Laser Altimeter (LOLA) data) for precision lunar topographic
modeling and analysis. A combined block adjustment model is developed for the integration of
Chang’E-2 imagery and LOLA data, in which the participants are the image orientation parameters,
the intra-strip tie points and the inter-strip tie points collected from the Chang’E-2 images, the
ground coordinates of the tie points, the LOLA ground points, and the back-projected image
coordinates of LOLA ground points. Two additional constraints are incorporated in the block
adjustment. One is a local surface constraint and the other is an orbit height constraint. The output of
the combined block adjustment is the improved image orientation parameters and improved ground
coordinates of the LOLA points, from which precision lunar topographic models can be derived.
15 strips of Chang’E-2 imagery and the corresponding LOLA data in the Sinus Iridum area on the
Moon are employed for experimental analysis. High precision digital topographic models including
digital elevation models (DEM) with spatial resolution of 20m and digital orthophotos with spatial
resolution of 7 m are generated in the Sinus Iridum area. Based on the generated topographic models,
detailed topographic analysis including slopes and distributions of craters are carried out and results
are presented.
CDMA-Based Same Beam Interferometry for Future Deep Space
Missions
Hao Wanhong1, M. Gregnanin
2, L. Iess
2, L. Simone
3
1 Beijing Institute of Tracking and Telecommunications Technology, Beijing, China
2 Dipartimento di Ingegneria Meccanica e Aerospaziale, Sapienza Università di Roma, Rome,Italy
3Thales Alenia Space Italy, Rome, Italy
Abstract: Our knowledge of the interior structure of solar system bodies is the key to the
understanding of their origin and evolution and relies almost entirely on gravity, rotation and, when
available, magnetic field measurements. Indeed, the accurate measurement of the rotational state and
tidal deformations of a celestial body, together with altimetric and gravitational field measurements,
provides strong constraints on its mass distribution and elastic properties against depth. In many
cases, in addition to the thickness and density of differentiated internal layers, one may also
determine their physical state, therefore revealing the presence of sub-surface oceans and fluid cores,
as in the case of Titan and Mercury.
Although measurements from orbit or from ground based radar have been essential to estimates of
the rotational parameters and the k2 Love number for several planetary bodies, much improved
accuracies can be attained by using landers or passive laser reflectors on the surface. These methods
have been used with extraordinary success in the Lunar Laser Ranging program. The upcoming
NASA’s INSIGHT Mars geophysical lander will also improve our knowledge of Mars’ rotation.
When networks of landers are available, several orders of magnitude improvements can be attained
by means of a powerful technique known as Same Beam Interferometry(SBI). In the context of
planetary geodesy, SBI is an interferometric tracking technique, consisting in the simultaneous
tracking in a coherent, two-way mode of two or more landers from a single ground antenna. The
downlink signals coming from each probe are combined to form the differential phase, which
contains information about the differential range of the two probes. In this configuration, due to the
small angular separation of the two beams, SBI contributes a great deal to cancel out common noise
sources in the two-way signal paths of each pair of probes, including solar plasma, ionospheric and
tropospheric delays, as well as other error sources, such as uncertainties in the station location,
thermo-mechanical deformations of the ground antenna, and errors in the Earth orientation
parameters.
The measurement of the differential phase delay allows the determination of the differential range to
the landers with unprecedented accuracy. Preliminary estimates show that, with a suitably designed
radio system, accuracies of the order of 0.2 mm can be attained for a lunar network, while for Mars
the accuracy can be of 1 mm. Some residual, systematic instrumental effects of the ground and
lander radio system must be carefully assessed and minimized. A very important source of systematic
effects is the frequency dependent phase delay in the ground receiving chain and the onboard
transponder. Indeed, the currently adopted configuration of the deep space radio links entails a single
and dedicated communication channel for each probe. While the separation in frequency prevents
interference between the telecomm and telecommunication channels of the landers, it exposes the
carriers used in the SBI to differential delays driven by the frequency-phase response of the
electronics. Those differential delays may be the limiting factor of the SBI measurements.
This limitation can be circumvented by adopting a communication architecture based upon Code
Division Multiple Access (CDMA). Spread spectrum radio links using pseudo noise (PN) codes
effectively spread the carrier power over a broad spectral region, therefore resembling a background
noise in the frequency domain. The signals to and from each lander of the network would be encoded
with different and unique PN codes, and effectively spread over the same bandwidth. This
architecture maximizes the signal commonality and reduces differential phase delays in the ground
and onboard electronics. CDMA communication channels are therefore the method of choice for SBI.
In addition, CDMA architectures would allow an optimal use of ground resources by enabling
simultaneous tracking, telecommandand telecommunications to all network landers from a single
ground antenna.
This work presents the analysis of a CDMA-based same-beam interferometer for the measurements
of the tides and rotational parameters of Mars and the Moon. In addition to the architectural
definition, link analysis, and acquisition strategies, we outline the benefits of such a system for the
investigation of the deep interior structure of those two bodies.
Error Characterization of Vision-based Detection and Tracking for
Spacecraft Navigation
Wei Shao
Qingdao University of Science& technology
Abstract: This paper focuses on the error characterization of spacecraft to achieve precision
planetary landing using feature tracking through a sequence of descent images. Using matrix
perturbation theory and covariance propagation, the error sensitivity of motion estimation with a
general model of image noise is provided. The analyticity of our results allows us to examine the
error sensitivity in terms of the translation direction, the viewing angle from the navigation camera.
The motion estimation uncertainty is shown in the experimental results, leading to better use of the
navigation method in engineering applications.
Understanding The Importance of Pickup Oxygen Ion Precipitation to
the Mars Upper Atmosphere
Xiaohua Fang1, Stephen Bougher
2, Robert Johnson
3, Janet Luhmann
4, Yingjuan Ma
5,
Yung-Ching Wang4, and Michael Liemohn
2
1Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, Colorado, USA
2Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, Ann Arbor,Michigan, USA
3Engineering Physics, University of Virginia, Charlottesville, Virginia, USA
4Space Sciences L aboratory, University of California, Berkeley, California, USA
5Institute of Geophysics and Planetary Physics, University of California, Los Angeles, California, USA
Abstract: While the Mars upper atmosphere is continuously bombarded by charged particles of solar
and planetary origins, the energy flux carried is often not sufficient to significantly affect the neutral
atmosphere. However, we show that this is not the case during major space weather events. By
applying two Mars global models -a Monte Carlo model for simulating pickup O+ precipitation at the
exobase and a thermosphere -ionosphere model for assessing its global impact, we find that the
thermospheric effects of reentering ions can change from negligible to very important when upstream
solar w ind conditions vary from normal to extreme. The atmospheric response under the most
extreme conditions includes dramatic neutral temperature enhancement, significant neutral
composition and wind changes, and increased importance of sputtering loss and possibly even
thermal escape of heavy species.
Harris Operator Feature Point Matching for Sequence Image of Mars
Landing Sites Based on FPGA
Qin Xu
Inst. Surveying and Mapping,China
Abstract: Feature point matching is essential for safe landing of Mars exploration mission. In view of
the efficiency, robustness and low power cost, FPGA is used in deep space exploration task.
Compared with other feature point matching operator such as SIFT and SURF, Harris operator has
the merits of both robustness and low computing complexity. In this paper, a Harris operator image
matching algorithm used for sequence image of Mars Landing Sites based on FPGA is proposed. In
order to improve the matching efficiency of image points and maintain robustness at the same time, a
32 dimension feature descriptor is built. Experiment result tested on Curiosity’s landing site – Gale
Creater demonstrates that our algorithm’s feasibility and efficiency.
Key Words: Mars; Mars Exploration; Image Matching; Harris Operator; FPGA
Molecular-Kinetic Simulations of Escape from The Ex- Planet and
Exoplanets: Criterion for TransonicFlow
Mau C.Wong3,1
, Robert E. Johnson1,2
, Alexey N. Volkov1, and Justin T. Erwin
1
1 Engineering Physics, University of Virginia, Charlottesville, VA 22904 USA
2 Physics Department, New York University, NY 10003 USA
3 Jet Propulsion Laboratory, California Institute of Technology, Pasadena CA 91109
Presenting and Correspondent Author: Mau C Wong; Email: [email protected]
Abstract: The equations of gas dynamics are extensively used to describe atmospheric loss from
solar system bodies and exoplanets even though the boundary conditions at infinity are not uniquely
defined. Using molecular ;kinetic simulations that correctly treat the transition from the continuum to
the rarefied region, we confirm that the energy ;limited escape approximation is valid when adiabatic
expansion is the dominant cooling process. However, this does not imply that the outflow goes sonic.
Rather large escape rates and concomitant adiabatic coo ling can produce atmospheres with subsonic
flow that are highly extended. Since this affects the heating rate of the upper atmosphere and the
interaction with external fields and plasma, we give a criterion for estimating when the outflow
goes transonic in the continuum region. This is applied to early terrestrial atmospheres, exoplanet
atmospheres, and the atmosphere of the ex;planet, Pluto, all of which have large escape rates.
Mars Science Laboratory Trajectory and Maneuver Analyses
Mau C. Wong and Julie A. Kangas
Jet Propulsion Laboratory, California Institute of Technology
4800 Oak Grove Drive, Pasadena CA 91109 USA
Presenting and Correspondent Author: Mau C. Wong; Email: [email protected]
Abstract: The NASA Mars Science Laboratory (MSL) rover, Curiosity, whose main goal was to
determine the habitability of the Martian environment, was launched on November 26, 2011 and
successfully landed at the Gale Crater on Mars on August 6, 2012. The design and execution of the
Trajectory Correction Maneuver (TCM) during the interplanetary phase have been documented in a
previous paper ( Wong et al., 2012). In this paper we will address trajectory and maneuver analyses
in the prelaunch design.
MSL was first scheduled to launch in November 2009 but was delayed to 2011 due to hardware
issues. Consequently, the entire process of target specification (launch/arrival date selection and
launch target generation), aimpoint-biasing (planetary protection requirements), and maneuver
analysis (propellant usage and delivery accuracies) was performed anew. A suite of hundreds of
plausible interplanetary trajectories was generated; even after the project had narrowed it to the
Type1 trajectory in August 2011, there remained about 70 plausible launch/arrival dates with each
of which tens of possible launch times within the launch window. The process of a complete
trajectory/maneuver analysis for each of these traje ctories involved a number of steps: 1) selecting
an biased injection aimpoint that would satisfy planetary protection requirements and minimize the
deterministic TCM -1 ΔV,2) specifying the launch targets for the launch vehicle, and 3) devising a
TCM targe ting strategy that would satisfy planetary protection requirements, spacecraft pointing
constraints, and propellant and delivery accuracy requirements.
Morphology Analysis of Lunar Craters Based on Multi- Source Data
ZHAO Jinjin1,2
, LIU Jianjun1, MU Lingli
1
1. National Astronomical Observatories of the Chinese Academy of Sciences, Beijing, 100012;
2. University of the Chinese Academy of Sciences, Beijing, 100049
Abstract: Morphological features of lunar craters vary in different areas of the lunar surface.
Distribution of lunar craters provides some formation of degenerative processes, as well as
geological and evolutional characteristics of the lunar surface. In this work, the morphological and
distributional characteristics of craters based on the lunar crater database LU60645GT and
Lunar_Impact_Crater_Database (2011) which compare with the DEM and DOM data of Chang'E-1
and Chang'E-2. The main findings are: 1) There are more craters with diameter (D) > 3km on the
farside of the Moon than those on the nearside. As for craters with D < 3km, the distribution is
reversed. 2) For fresh craters which depth(d) to diameter ratio d/D relatively high to those crater's
scale are the same, when D < 15km, the linear relationship between the depth and the diameter is
strong. For craters > 15km in diameter, the relationship between d/D and D is an exponential
function. 3) The average d/D ratio of craters in the highland regions is always larger than those in the
mare regions. 4) The d/D ratio is an insufficient parameter to describe the morphological features of
degenerated craters; instead the distribution function of depth-percentage to accumulative
area-percentage can better characterize the degenerated craters in the lunar mare regions.
Key words: Lunar impact crater; Morphological features; Geometrical shape; Distribution;
Differences; Degenerate
Global Hybrid Kinetic Simulations and Comparison with
MESSENGER
Jan Paral1 and Robert Rankin
2
1 Department of Physics and Astronomy, Dartmouth College, Hanover, NH 03755-3528, USA.
2 Department of Physics, University of Alberta, Edmonton, Alberta, Canada T6G 2G7.
Abstract: The NASA MESSENGER spacecraft entered orbital phase around Mercury on March 18,
2011. A surprising consistent feature in the data returned is the occurrence of large-scale vortices that
form exclusively on the dusk side of the magnetosphere. Here, we present global kinetic-hybrid
simulations that explain these observations. It is shown that vortices are excited by a
Kelvin-Helmholtz instability near the subsolar point, which grows convectively along the dusk-side
magnetopause. Virtual time series along a track approximating a flyby of MESSENGER show
correspondence with the satellite data: the data contain sawtooth oscillations in plasma density, flow,
and magnetic field, and exhibit the observed dawn-dusk asymmetry. It is shown that asymmetry
between dawn and dusk at Mercury is controlled by the finite gyro-radius of ions, and by convection
electric fields. It is further demonstrated that asymmetry on the dawn side manifests through gradient
initiated pressure disruption of the flow, which produces bubbles of plasma that are suggestive of
fluid instabilities such as the Rayleigh-Taylor instability.
Jovian Impact Flashes and their Implication to Small Solar System
Bodies
Junichi WATANABE1, Isshi TABE
2
1 National Astronomical Observatory of Japan, Japan,
2 Libra Co., Japan
Corresponding author: [email protected]
Abstract: Optical flashes on the surface of Jupiter were observed by amateur astronomers in June
and August 2010. Especially latter case was observed by four amateur astronomers in Japan. The
duration of the flash was about two seconds, and the brightness was 6.2 magnitudes. This is
presumed to be an equivalent or slightly smaller scale than that in June. These phenomena were
bright meteors caused by the collision of small celestial bodies of a few to 10 m. If the frequency and
the scale of these phenomena are investigated, the size distribution down to size of a few m can be
estimated at around the giant planet region.
In case of Earth, the brightness of meteors depends not only on sizes but also on the entry velocity.
However, in the case of Jupiter, the entry velocity becomes almost similar value (60-64km per
second) which is almost independent on the impacting direction. We do not have any uncertainty for
estimating size of impacting bodies from the brightness of the flashes.
On the other hand, we have large uncertainty in the size distribution of small bodies in the giant
planet region [3], because we cannot see directly any bodies of less than 1 km. Therefore, if the
systematic observation is achieved, it will be a unique attempt to use the giant planets as a natural
detector of small bodies, and to derive size distribution of small bodies in the giant planet region.
For this purpose, we coordinated both professional and amateur astronomers in Japan and China, and
performed monitoring campaign in September and November 2012. In this paper, we present the
results of these campaign observations.
Influence of the atmosphere and ocean on the resonant polar motion
Leonid Zotov1, Christian Bizouard
2
1 Sternberg Astronomical Institute, Lomonosov Moscow State University, Russia
2 IERS Earth Orientation Parameter Center, Paris Observatory, France
Abstract: Observed motion of the Earth’s rotation axis exhibits mostly two resonances. One is the
resonance of the polar motion with respect to the Earth's surface, at the Chandler frequency of 0.843
cycles per year. On the other hand the oscillation of the rotation axis with respect to stars, the
so-called precession-nutation, possess a resonance at 0.849 cycle per year, and is attributed to the
Free Core Nutation (FCN).
Many studies are devoted to the clarification of the excitation sources at the resonant frequencies.
The problem is difficult in the sence that resonant polar motion or precession-nutation are caused by
small excitations of which the amplitude is just above the uncertainty.
The problem is first approached by the inverse problem solving: reconstructing of the geodetic
excitation from rotation pole observations. Here regularization techniques should be used.
On the other hand excitation is modeled on a physical basis, considering the contribution of the
oceans, atmosphere, and fresh water trough the angular momentum variations.
More or less extended series of angular momentum (~50 years) are available for ocean (OAM) and
atmosphere (AAM), so that the effect of these fluid layers on the Earth rotation has been widely
studied.
But mass redistribution taking place in atmosphere and ocean, are themselves subjects to the
influence of various processes, of geophysical, astronomical and even anthropogenic nature. We
expect that they are amplified at the resonance frequencies, and therefore we can try to track them in
the Chandler and FCN band.
Using specially designed narrow-band Panteleev filter, we reconstruct geodetic excitation on the
Chandler and FCN frequencies. We compare it with the oceanic and atmospheric ones not only
globally, but also regionally, using longitude-latitude maps of the angular momentum distribution for
ocean and atmosphere, mass and motion terms.
The attempt of such comparison is also done in the frame of new generalized model of Bizouard.,
which takes into account triaxiality of the Earth and asymmetry of the ocean tide.
Calculations of the Lunar Surface Electrical Field for the Estimations
of Moon Dust and its Distributions for Future Lunar Explorations
Dr. Yunlong Lin
Project Scientist, Department of Mechanical and Aerospace Engineering,
University of California, Davis, One Shields Avenue, Davis, CA, 95616
Email: [email protected]
Abstract: The moon dust and surface electrical field estimations are important to future human and
robotic activities on the surface of the moon. Apollo astronauts had witnessed the maintaining of
micron- and millimeter sized moon dust up to meters level while walked on the surface of the moon.
The characterizations of the moon dust would enhance not only the scientific understanding of the
moon but also the future technology development for the surface operations on the moon. It has been
proposed that the maintaining and/or settlement of the small-sized dry dust are related to the size and
weight of the dust particles, the level of the surface electrical fields on the moon, and the impaction
and interaction between lunar regolith and the solar particles. The moon dust distributions and
settlements obviously affected the safety of long term operations of future lunar facilities. Through
analyzing the imaging of the legs of the moon lander, the cover and the footwear of the space suits,
and the envelope of the lunar mobiles, we estimated the size and charges associated with the small
moon dust particles, the gravity and charging effects to them along with the lunar surface
environment. In this Paper, we present the calculations of the lunar surface electrical fields due to
the impaction of the solar winds in several conditions, and the results showed that the maintaining of
meters height of the micron size of moon dust is well related to the electrical field and the solar angle
variations, as expected. These results could be verified and validated through on site and/or remote
sensing measurements and observations of the moon dust and the surface electrical field in future
moon exploration missions.
3D Reconstruction of Vesta From Sequence Image of DAWN Based on
Multi-view dense Matching Algorithm
LAN Chaozhen1,2
,GENG Xun1,3
, HOU Yifan1
1 Institute of Geographic Space Information, Information Engineering University, Zhengzhou 450052, China;
2 School of Aerospace Engineering, Beijing Institute of Technology , Beijing, 100081,China; 3 Xi’an Institute of Surveying and Mapping Information Technology, Xi’an 710054, China;
Abstract: With sequence image acquired from NASA’ asteroid exploration mission—DAWN, the 3D
topographic reconstruction of Vesta based on mutli-view dense matching algorithm is researched.
Firstly, the geometric parameters of the frame camera on DAWN including focal length, principal
point of photograph and optical distortion are calibrated. Then the sequence images are epipolar
resampled which is essential for dense matching. Thirdly, multi-view dense image matching
algorithm based on the geometric constraints of epipoar line is used to extract corresponding points
and the 3D topographic information of Vesta can be reconstructed. Experiment results demonstrate
that our method can reconstruct the 3D topographic information of Vesta even if the geometric
parameter of the frame camera is not known accurately.
Keyword: deep space exploration; asteroid; DAWN; Vesta; 3D reconstruction; Image Matching
The follow-up observations of several exoplanet transit events
Liyun Zhang & Qingfeng Pi
Guizhou University, China
Abstract: We present new photometric data of the transiting planet HAT-P-20b, HAT-P-25b, and
WASP36 by using 85-cm telescope of Xinglong station of the National Astronomical Observatories
of China in 2012.Our new transit curves are modelled using the JKTEBOP code and adopting the
quadratic limb-darkening law. We determine the improved ephemeris with a transit epoch, and
discuss a period change by the observed minimum minus calculated transit times. The primarily
parameters (the orbital inclination, radius ……) of these star-planet system are revised. Finally, we
give the future plan on this research topic in China.
Venus upper clouds; morphology, dynamics and physical properties
Wojciech J. Markiewicz1, Dimitri Titov
2, Elena Petrova
3, Nikolay Ignatiev
3, Igor Khatuntsev
3, Sanjay S. Limaye
4,
Oksana Shalygina1, Eugene Shalygin
1 and the VMC team.
1 Max Planck Institute for Solar System Research, Germany,
2 European Space Agency/ESTEC, Holland,
3 Space Research institute/IKI, Russia,
4 University of Wisconsin, USA.
Abstract: The Venus Monitoring Camera(VMC) on Venus Express(VEX) spacecraft has been
observing the upper cloud layer since April 2006. To date more than three hundred thousand images
have been acquired. VEX has a highly elliptical orbit allowing for global as well as close up views
with resolution down to 200 meter per pixel. The VMC is a CCD camera with four channels in the
UV, visible and near IR, with centre wavelengths at 365, 513, 965 and 1010 nanometers
respectively. The VMC UV wavelength corresponds to the spectral feature of a so far unidentified
absorber. In particular this subset of the VMC data shows greatvariety of morphologies. On global
scales these include equatorial belts, bright polar bands and polar caps. The observed small scale
features change their appearance from mottled clouds and convective cells at low latitudes to
streaky patterns at middle and high latitudes. Time sequences of global views have been used
extensively to track clouds and hence to obtain wind speed vectors. Many of the morphological
features we see in UV channel are also visible in other wavelengths. As the VEX spacecraft comes
closer to the planet we no longer monitor cloud motion and rather quickly fly over them. During
these pericentre passages it is possible to make dayside mosaics of the clouds as well as night side
mosaics of the surface. The pericentre passage allows for the highest resolution images. Some of the
most interesting ones are found in the equatorial convective region. The scales of the cells go down
to few tens of kilometers and are significantly smaller than observed previously. This may have
implications for the thickness of the convective zone itself and hence provide clues for
understanding the difficult problem of vertical transport of energy and momentum. In near polar
regions, usually above 50° latitude, we see many waves. These are most likely gravity waves and are
visible in all four VMC channels. By modeling phase dependence of brightness in the VMC data in
all channels we can infer the physical properties of the upper clouds as well as the haze which in
most cases lies
above the clouds. Most recently we have observed and analyzed images of the glory on the top of the
clouds. These data constrain physical properties of the droplets and are the first observations of a full
glory outside of the Earth environment.
Dawn at Vesta: picture of a protoplanet
M.T. Capria, C.T. Russel, C.A. Raymond, E. Ammannito, F. Capaccioni, U. Christensen, M.C. De Sanctis, B.
Feldman, R. Jaumann, H.U. Keller, T. McCord, L. McFadden, H. McSween, S. Mottola, A. Nathues, G. Neukum, C.
Pieters, T. Prettyman, H. Sierks, M. Sykes, M. Zuber and the international Dawn team
Abstract: The NASA mission Dawn was launched on September 27, 2007 and reached Vesta on July
16, 2011. Dawn orbited Vesta until September 2012, and then departed for Ceres, where it will arrive
in early 2015. Vesta, a big, differentiated body orbiting the Main Asteroid Belt, was fully
characterized by the mission. The exploration gave many surprises, letting us know a fascinating
diversity of terrains and features visible on its surface. This talk will review the main findings of
Dawn, illustrating what we know know about Vesta also with respect to the history of the Solar
System.
Navigation Fusing a Single Optical Observation with a
Single Pulsar Based on Observability Analysis
Dayi Wang, Maodeng Li, Xiangyu Huang
National Laboratory of Space Intelligent Control, Beijing Institute of Control
Engineering, Beijing, 100190, China
Abstract: An observability analysis for navigation using either a single line of sight
optical measurement or a single X-ray pulsar is performed. The analysis involves
eigenvalue/eigenvector decompositions of the fish information matrix using Cramer-Rao inequality.
The informationmatrix is shown to be singular when only one observation is obtained, which
indicates that the system is un-observable. An analysis is also performed to study the observability
for navigation system using a single optical beacon together with a single pulsar. Based on analytical
solutions of eigenvalues and eigenvectors of the covariance matrix, it is shown that the most
observability can be achieved if the line of sight to the optical beacon is parallel tothe pulsar. This
observability analysis is then used to design fusion architectures for optical/X-ray pulsar integrated
navigation to enhance navigation performance. The high performance of the integrated navigation is
illustrated through numerical simulations in comparison with the method using a single optical
beacon or pulsar.
Keywords: Cramer-Rao lower bound(CRLB), optical/X-ray pulsar integrated navigation,
observability analysis
VLBI Astrometry, Rotation, Physical Libration and Interior Structure
of the Moon for «LUNA-GLOB» and «LUNA RESOURCE» Russian
space missions (2015-2017yrs)
Alexander Gusev
Kazan Univ., Russia
Abstract: Many space agencies plan a lunar missions, including observations in the near lunar space
and/or on the surface of the Moon. One of these projects of “I-VLBI” propose to place two landers
with radio beacons on the Lunar near side and to launch one or more Orbiters on the Lunar orbit .
The difference of the distances between two radio beacons and Earth will be assumed to be measured
by the methods of Inverse VLBI: radio-signal from the various radio beacons will be sent to Earth
antenna systems using the Orbiter. The estimation of the physicallibration angle accuracy is made for
various location and configuration of the radio beacons, which are in polar or equatorial zones of the
Moon.
The planned accuracy of difference distance determination for radio beacons at 60- 100 mm and the
length of base line of 1700-3400 km in the Inverse VLBI experiment will be sufficient to improve
accuracy of lunar physical libration, better than 10- 30 msec of arc. Analogous estimation of
latitude libration has shown the same results: location of the Radio Beacon I and Radio Beacon II in
the vicinity of the lunar limb equator and the prime meridian will give the best estimations for the
physical libration angeles. For radio beacons experiment the best accuracy of longitudinal and
latitudinal librations (10 - 30 msec of arc) will be achieved in the equatorial limb and polar zones of
the Moon.
SPACE DEBRIS: ITS ALARMING STATE
NishantArora
B.Tech, Department of Electronics & Communication Engineering
Institute of Science & Technology, Klawad, Haryana, India
Email:[email protected]
Abstract: Space debris has become a growing concern in recent years, since collisions at orbital
velocities can be highly damaging to functioning satellites and can also result into more space debris.
Some spacecraft, like the International Space Station, are now armored to deal with this hazard.
Armor and mitigation measures make satellites or human spaceflight vehicles like the shuttles very
expensive and heavy. This paper is a semi-technical survey of the expanding literature of the
subject. The paper explores the different sources and mitigation methods of space debris. I have
proposed some methods to deal with this problem of space debris. I have also highlighted the
shortcomings of some of the proposed methods found in the literature and I have further proposed
some modifications in some of those methods. I feel some of them can be very effective in the
process of mitigation of space debris; few of them may need some modifications. The paper proposes
the use of nanobot and nanotube mesh technique, the use of decayable material for manufacturing of
space machines and I suggest the proper segregation and decomposition of the space debris and use
of some it for energy generation and space structure also.
Keywords: Space debris mitigation, orbit, nano mesh, nanobots and fuel cell.
A review of the main results from the VIS- IR imaging spectrometer
VIRTIS on board Venus Express
G. Piccioni1, P. Drossart
2 and the VIRTIS-Venus Express Team
1 IAPS-INAF, via del Fosso del Cavaliere, 100, 00133, Rome, Italy
2 LESIA , 5, place Jules Janssen, 92195 Meudon, Paris, France
Abstract: After more than six years since the orbit insertion, VIRTIS aboard the Venus Express
spacecraft has addressed a significant amount of the planned scientific objectives and also other
unexpected results, from the surface up to the upper atmosphere, in terms of mapping, composition,
structure and dynamics.
The VIRTIS instrument consists of two channels: VIRTIS-M, animaging spectrometer with moderate
spectral resolution in the range from 0.25 to 5.2 microns and VIRTIS-H, a high spectral resolution
spectrometer in the range from 2 to 5 microns co -aligned with the field of view of –M. The
resolution of VIRTIS-M is 2 nm from 0.25 to 1 microns, and 10 nm from 1 to 5.2 microns. The
resolution of VIRTIS -H is about 2 nm.
The atmosphere above the clouds is observed both on day and night sides, in solar reflection and
thermal emission in nadir geometry. Limb observations provide O2, OH, NO, CO2 and CO emissions,
through nightglow and fluorescence observations. Spectroscopy of the 4 -5 micron range gives
access to the cloud structure in the 60-95 km alt itude levels.
The deeper atmospheric windows, limited by CO2 and H2O bands are accessible only in thermal
emission on the night side. The sounded levels at 1.7 and 2.3 microns are limited respectively to
30-20 km altitude, while at shorter wavelengths (1. 18, 1.10, 1.01, 0.9 and 0.85 microns), the hot
surface of Venus is seen through the scattering clouds.
Multiwavelength clouds tracking and thermal fields allow studying the wind fields and the global
dynamics, in particular the complex details of the polar vortex.
A brief description of the instrument and a short review of the main results are reported in this paper.
Proposal for a Mission to Uranus
Chit Hong Yam, Kwing Lam Chan, Hermanni Heimonen
Department of Mathematics and Center for Space Science Research, Hong Kong University of Science and
Technology
Abstract : Uranus is the 7th planet of the solar system and closest of the two not yet visited by a
space orbiter. While it is gaseous, its atmospheric composition is notably different from those of
the two inner gas giants (Jupiter and Saturn). Compared to those on Jupiter and Saturn, its equatorial
wind is stronger but blows in opposition direction (retrograde vs. prograde). There are a large
number of scientific issues (e.g. off-center magnetic axis, icy composition, retrograde zonal winds,
long-lived spots) that await investigation by an orbiter mission to this planet. In this presentation,
we’ll show results of a global search for gravity-assist trajectories to Uranus with various flyby
sequences. We illustrate how the highly oblique equatorial plane of Uranus can affect the geometry
of the capture orbit and the touring in the Uranian system. We will also discuss the design elements
of a mission to Uranus and propose some candidate launch windows with low propellant costs and
acceptable flight times.
Fig.1 An example of gravity-assisted trajectory to Uranus
Japanese atmospheric escape mission to Mars (heir of NOZOMI): Role
of atmospheric escape in evolution of Martian environment
K. SEKI1, A. MATSUOKA
2, N. TERADA
3, T. ABE
2, A. YAMAZAKI
2,
S. YOKOTA2, M. HIRAHARA
1, T. IMAMURA
2, H. HAYAKAWA
2,
and Martian Atmospheric Escape Mission Working Group 1 Solar-Terrestrial Environment Laboratory, Nagoya University, Aichi 464-8601, Japan
2 Institute of Space and Astronautical Science, JAXA, Kanagawa, Japan
3 Graduate School of Science, Tohoku University, Sendai, Miyagi, Japan
Abstract: The cumulative effect of the atmospheric erosion due to the external forcing is regarded as
one of the plausible candidates of the drastic climate change from warm and wet to cold and dry
environment, which Mars is believed to have undergone in the past. Our target is to elucidate
non-thermal escape processes, in particular, solar wind-induced escape processes, which are pointed
out to involve substantial uncertainties by previous measurements and theoretical studies. This target
was one of the main scientific objectives of Nozomi (launched in 1998), the Japanese first mission to
Mars. Recent progress made by MGS and Mars Express has given us partial view of current
atmospheric escape, and the motivation is now taken over by the upcoming MAVEN mission of
NASA. MAVEN is planning to carry out a comprehensive in-situ observation of the atmospheric
escape, which will unveil the current state of upper atmosphere and its escape.
The Martian atmospheric escape mission working group at ISAS/JAXA has studied possibility of
two-orbiter mission in order to deepen our understanding of escape processes and their response to
the solar variations to the level of an extendable one to the past to discuss atmospheric evolution,
which cannot be achieved by one satellite. We consider that the following combination of remote
sensing and in-situ measurements from two orbiters is essential to get key information. Simultaneous
observations from the “high-altitude orbiter”, which will grasp a global (planet-wide) structure of
escaping ions and neutrals by UV/EUV/VIS imaging, and from the “low-altitude orbiter”, which will
investigate the escape processes by in-situ measurements, enable us to identify many essential escape
processes. In addition, the imaging as well as the high-mass-resolution in-situ particle measurements
can identify ion and neutral compositions of escaping atmosphere related to CO2. It will enable us to
study how much the greenhouse gas has escaped from Mars. The “high-altitude orbiter” also
provides another key observation: solar wind and radiation monitoring. The solar wind monitoring is
crucial to precisely understand present escape processes/fluxes as well as their dependences on the
external conditions of the solar activity, which are necessary to reconstruct the evolutional history of
atmospheric escape with geological timescale. The mission will also carry atmospheric imagers
dedicated to the coupling of lower and upper atmosphere to address the effects of lower atmospheric
dynamics on the atmospheric escape from Mars.
Effects of the surface conductivity and IMF strength on dynamics of
planetary ions in Mercury’s magnetosphere
K. SEKI1, N. TERADA
2, M. YAGI
2, D. C. DELCOURT
3, F. LEBLANC
4,
and T. OGINO1
1Solar-Terrestrial Environment Laboratory, Nagoya University, Aichi 464-8601, Japan
2Graduate School of Science, Tohoku University, Sendai, Miyagi, Japan
3LPP-CNRS, 94107 - Saint Maur des Fosses, France
4LATMOS, CNRS, UPMC 4 place Jussieu 75005 Paris, France
Abstract: A previous study of ion dynamics in the Mercury's magnetosphere, which uses a rescaled
analytical model of the geomagnetic and electric fields for Mercury, shows that non-adiabatic motion
of ions in the magnetotail can cause a narrow band of energetic (several keV) Na+ precipitation in
each hemisphere [Delcourt et al., 2003]. On the other hand, it is not evident that the
magnetospheric configuration and global convection pattern in the Mercury's magnetosphere can be
described with the rescaled geomagnetospheric model. In order to investigate whether the ion
dynamics in the self-consistent field configuration differs from that in the rescaled model, we
conducted systematic trajectory tracings of Na+ ions in the electric and magnetic fields obtained
from MHD simulations of the Mercury-solar wind interaction.
Comparison with a previous study, which used an analytical model by rescaling Earth's
magnetosphere and assumed the existence of the distant neutral line (DNL) in Mercury's magnetotail,
shows the drastic change in Na+ precipitation pattern onto due to formation of the near-Mercury
neutral line (NMNL) in MHD simulations. Na+ precipitation band around 30 degrees of latitude
(LAT) obtained in the previous study disappeared in the equivalent low-conductivity MHD case due
to the NMNL formation, while the NMNL formation causes high-energy Na+ precipitation into
equatorial region. The change in the strength of the southward IMF (sBz) alters the location of
NMNL and Na+ precipitation pattern. In the low-conductivity sBz=5 case, both the equatorial
precipitation and Na+ band around LAT=30 are formed. In the high-conductivity sBz=5 case, on one
hand, magnetospheric convection through polar regions is suppressed and it results in a region of
dense Na+ near the planet. These results suggest that the dynamics of planetary ions in the
magnetosphere of Mercury and related precipitation onto the planet surface change significantly with
the activity level of Mercury's magnetosphere. It is also suggested that we can gather information
about the surface conductivity from observations of either the magnetospheric convection,
distribution of Na+ ions around the planet, or precipitation pattern of Na+ ions onto the planetary
surface.
Planetary Evolution and Life: Astrobiology from a Planetary Science
Perspective
Tilman Spohn
DLR Institute of Planetary Research, Berlin
Abstract: The habitability of planets has received increasing interest in recent years, in particular in
view of the increasing number of detected extrasolar planets. Planetary habitability (for life as we
know it) is usually thought to require water on (or near) the surface and a sufficient supply of energy
and nutrients. The request for water on the surface leads to the concept of the habitable zone where
stellar radiation and atmosphere greenhousing keep the surface temperature within the stability range
of liquid water. A magnetic field is argued to serve to protect an existing atmosphere against erosion
by the stellar wind and thus to help stabilize the presence of water and habitability. Present theories
of the origin of life on Earth and an early chemotrophic biosphere require volcanic activity and the
associated large thermal gradients as energy and entropy sources. Magnetic fields are generated in
the cores of terrestrial planets and thus habitability is linked to the evolution of the interior through
magnetic field generation and volcanic activity. Moreover, the interior is a potential source and sink
for water and other greenhouse gases and may interact with the surface and atmosphere reservoirs
through volcanic activity and recycling. The most efficient known mechanism for recycling is plate
tectonics. On the Earth, surface water is stabilized by complex interactions between the atmosphere,
the biosphere, the oceans, the crust, and the deep interior in the carbon-silicate cycle for which plate
tectonics is a central element. But plate tectonics is widely believed to require water in the mantle to
operate and it can thus be argued that plate tectonics is an element linking the biosphere to the
evolution of the planet’s interior. Previous studies have proposed that life (together with plate
tectonics) has caused a change in the redox-state of the mantle and provided a path for continent
formation. We present numerical model that relates bioactivity and plate tectonics to the growth of
the continental surface area of the Earth and to the hydration state of the mantle. The link is provided
by assuming that bioactivity causes an increase in erosion of continental crust as compared to a
putative abiotic Earth and an increase in the thickness of the sedimentary layer on top of a
subducting oceanic slab. As the sedimentary layer is usually of lower permeability than the oceanic
crust more water is subducted per unit volume and time. This in turn leads to a greater availability of
water in the source region of andesitic partial melt, resulting in an enhanced rate of continental
production, and an enhanced regassing rate of the mantle. Our results suggest that a biologically
increased weathering rate not only results in a more hydrated mantle but also in a larger continental
surface area. If the presence of life has increased continental weathering over time, as is widely
believed, we conclude that Earth-like planets lacking life would have a dry mantle, may lack
continents and possibly even plate tectonics altogether.
The Moon: collars of beads in and around the Mare Orientale make
questionable its widely cited impact origin
Kochemasov G. G.
IGEM of the Russian Academy of Sciences, 35 Staromonetny, 119017 Moscow, [email protected]
Abstract: The wave planetology implies that along with some impact features on planetary surfaces
prevail roundish forms of non-impact origin. Intersecting standing inertia-gravity waves, origin of
which is related to keplerian non-round orbits with changing accelerations, make them. Warping
waves in rotating bodies have four interfering ortho- and diagonal directions (Fig. 2). The NASA’
GRAIL mission has provided excellent gravity maps of the lunar marea and basins showing regularly
spacing zones of differing gravity and composing them “craters” –beads (Fig. 1). The best
explanation of their origin by the wave model is in Fig. 2. The Kaguya gravity anomalies (Fig. 3)
show intersecting chains and grids of even-sized shoulder-to-shoulder “craters” of the wave origin.
1 2
3
“Frequency-dependence of the tidal dissipation on the Moon: Effect of
the low-viscosity zone at the lowermost mantle”
Yuji Harada 1, 2
, Sander Goossens 3, Koji Matsumoto
4, Jianguo Yan
5, Jinsong Ping
6, Hirotomo Noda
4, Junichi
Haruyama 7
1 Panetary Science Institute, Faculty of Earth Sciences, China University of Geosciences, Wuhan, China
2 Division of Earth and Planetary Materials Science, Earthquake Research Institute, the University of Tokyo, Japan
3 Planetary Geodynamics Laboratory, Goddard Space Flight Center, National Aeronautics and Space
Administration, USA 4
RISE Project Office, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, Japan 5 Division of Precise Spatial Positioning, State Key Laboratory of Information Engineering in Surveying, Mapping
and Remote Sensing, Wuhan University, China 6 Research Division of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese
Academy of Sciences, China
7 Department of Solar System Sciences, Institute of Space and Aeronautical Science, Japan Aerospace Exploration
Agency, Japan
Abstract: Tidal energy dissipation on a solid planetary body is generally one of the important
geophysical phenomena. Primarily, tidal dissipation depends on its internal structure, especially
viscosity structure, and therefore, constrains its interior. Furthermore, tidal heating or viscosity
distribution inside a planetary interior connects with its thermal and orbital states, which possibly
provides some constraints on thermal and orbital evolution as well. The Moon is not an exception.
Although there are a few previous examples of model calculation to deal with dependence of the
tidal dissipation on the lunar interior structure, it is still hard to say that any of these studies has been
able to explain the frequency-dependence of the actual tidal dissipation derived from the geodetic
observation. In particular, the quality factor obtained from the continuing lunar laser ranging for
many years indicates the weak frequency-dependence. However, the conventional model calculation
has not completely explained the observed frequency-dependence, or in the first place, has
disregarded this dependence.
It is significant in the viewpoint of lunar science to resolve the above-mentioned problem on the
frequency-dependence. At least, finding out some internal structure consistent with this dependence
is practically the same as imposing some additional constraint on the internal structure. In addition to
the interior structure, it might be possible even to give implications to reconstruct its histories, such
as thermal and orbital evolution.
In order to explain frequency-dependence here, careful attention should be paid to the influence of
the low-viscosity layer inside the mantle. It is already known that, based on the moonquake, the
strong seismic attenuation zone exists at the bottom of the lunar mantle. The existence of this high
attenuation zone implies that the viscosity of the lowermost part of the mantle is lower compared to
the upper one. If so, this dependence would be explainable by taking the impact of the lowermost
portion on the tidal dissipation into account, which has not been examined in the previous works.
In the present study, in order to estimate the effect of the low-viscosity zone at the lowermost mantle
exerted on the frequency-dependence of the tidal dissipation on the Moon quantitatively, model
calculation of the viscoelastic tidal deformation was performed with respect to the monthly and
annual periods. Here the seismologically-derived internal structure is given concerning the density
and elasticity structure. Concerning the viscosity structure, on the other hand, although not only the
existence of the low-viscosity layer but also those of the lithosphere and asthenosphere is taken into
consideration, only the viscosity value of the low-viscosity layer is adjusted while those of the
remaining two layers are regarded as uniform and constant. Moreover, the mechanical constitutive
relation in this calculation follows the rheological law of Maxwell body. And finally, the interior
structure, particularly the viscosity of this specific zone is determined by comparing the present
numerical result with the preexisting observational result.
As a result of the present calculation, the additional influence of the low-viscosity layer successfully
provides the viscosity structure which has no inconsistency with the geodetic observables on the tidal
dissipation. More specifically, its viscosity satisfies the quality factor derived from the lunar laser
ranging for both monthly and annual periods. This viscosity value is extremely low, which Maxwell
relaxation time is close to the tidal periods. Also, the theoretical range of the complex tidal Love
number corresponding to this viscosity structure restricted through the quality factor almost
corresponds at the same time to the observational range based on the precision orbit determination of
the historical lunar orbiters.
This result reveals that, as far as the low-viscosity layer is assumed to exist, even such simple linear
rheology can easily interpret the frequency-dependence of the lunar tidal dissipation. One of the
former attempts suggested that the observed frequency-dependence on the tidal dissipation is not
necessarily interpretable even if following, instead of the Maxwell model, more complicated
rheological model like the Burgers model. However, the low-viscosity layer as a simple and natural
precondition leads to the different suggestion.
The conclusion obtained from the present result is that the low-viscosity layer certainly exists at the
lowermost part of the lunar mantle, and also that this layer induces tidal energy dissipation very
effectively. The most important knowledge clarified through this work is that the high seismic
attenuation zone is equivalent also to the low-viscosity zone. That is, it is thought that the portion of
exceedingly low viscosity exists adjacent to the core-mantle boundary on the Moon as well as on the
Earth. The fact that the relaxation time of this ultralow-viscosity zone is close to the tidal periods
means that the tidal heating is nearly the maximum within the range of the internal structure defined
in the above calculation. Moreover, there is a possibility that partial melting occurs in the deeper part
as has previously been pointed out. Perhaps substantial amount of melt is created, even suggesting
the rheologically critical state.
The present conclusion gives the further implication to thermal and orbital evolution on the Moon.
Above all, it deserves a special remark that the tidal dissipation is localized just inside the
low-viscosity layer. In other words, it is expected that the low-viscosity layer plays a role as a
blanket for the cooling of the core. Consequently, this layer should have an impact similar to the
layer of the ilmenite-rich cumulates which is rich in radioactive species. Furthermore, such tidal
heating in the low-viscosity layer may be balanced by heat transport due to mantle convection plus,
if partial melt-bearing, melt segregation. It is considered that this balance would choose optimal
viscosity which maintains the energy balance via self-regulation mechanism. This kind of thermal
history is governed by the orbital history on the Moon. Because tidal evolution gradually changes
amplitudes and periods of tidal potential, the viscosity and the temperature in the mantle would also
reflects these variations accordingly.
PROBABLE SIGNS OF THE CLOUDS VERTICAL
INHOMOGENEITY ON JUPITER
Tejfel V.G. , Kharitonova G.A.
Fessenkov Astrophysical Institute, Almaty, Kazakhstan
[email protected], [email protected]
Abstract: In November and December 1999 special observations of Jupiter were carried out for
detailed study on latitudinal and longitudinal variations of the absorption bands of CH4, centered on
619, 725, 798 and 887 nm. 388 CCD-spectrograms of the central meridian of Jupiter were recorded
and processed. During four nights all longitudes were observed twice with the step 1.8 degrees on
longitude. In this work some latitudinal differences of the behavior of the absorption in the CH4
619 and 725 nm bands are compared. The relatively weak band at 619 nm CH4 over all observations
has a maximum value Rv just south of the equator, at a latitude of about -5 degrees. The depth of 725
nm band shows a clearly expressed absorption maxima at latitudes of about -18 and +23 degrees and
with a minimum at about 4 degrees latitude. For other observation dates the view of graphics is
identical. The comparison of the 619 and 725 nm bands depths shows for all data a loop at low
latitudes -25 to +25 degrees and significant difference in their latitudinal variations. The
discrepancy between the positions of maximum and minimum absorption for the weak band 619 nm
and of stronger band at 725 nm may be considered as a result of different effective levels where the
absorption formed inside the cloud layer. If the vertical inhomogeneity of the cloud particles
distribution varied with latitude it must be seen in the latitudinal differences of the absorption bands
intensity. If the observed variations were due to absorption inhomogeneities in the atmosphere above
the clouds, for example, in the stratospheric layer of haze, the effect should be expressed more or less
equally in both bands. As a simple model for the interpretation of the observed latitudinal differences,
we used a two-layer model with semi-infinite cloud layer and pure gas atmosphere above the clouds.
For the cloud layer Henyey-Greenstein scattering function with the asymmetry parameter g = 0.75
has been adopted The reflectivity in the continuous spectrum of the cloud layer is assumed to be
0.75 . Calculations were based on the numerical data tables for the reflection in the absorption bands,
and to calculate the effective optical depth of the absorption formation. Discrete tabular data were
approximated with good accuracy by polynomials that allowed to make the calculations for all values
of the arguments. The absorption coefficients for the centers of the bands 619 and 725 nm were taken
from [4], the methane abundance in the atmosphere above the clouds Cm ranged from 0.001 to 0.02
km-amagat.The difference of effective optical depths for two bands may characterize the degree of
vertical inhomogeneity of the cloud layer at different latitudes. It is interesting that the minimum
degree of inhomogeneity falls on the equatorial zone. Of course, these results should be considered
preliminary and subject to verification by the data of further observations.
“A time scale of true polar wander on a quasi-fluid planet: Effect of a
low-viscosity layer inside a mantle”
Yuji Harada 1,2
Long Xiao1
1 Planetary Science Institute, Faculty of Earth Sciences, China University of Geosciences, Wuhan, China
2 Division of Earth and Planetary Materials Science, Earthquake Research Institute, University of Tokyo, Japan
Abstract: Although not so many, a few theoretical and numerical studies for large-scale true polar
wander on a solid planetary body has already been demonstrated. Besides these approaches, true
polar wander on some real planets, such as the Earth and Mars, has also been inferred from lines of
circumstantial evidence particularly in terms of geology, including paleomagnetism, whose scenarios
can be interpreted based on dynamical modeling like mentioned above.
In the previous modeling, however, heterogeneity on viscosity structure of a mantle, especially a
potential impact of a low-viscosity layer, has not necessarily been dealt with. In fact, for example,
geophysical observations recently tell us a possibility that the Earth interior includes layers with
extremely low viscosity inside the mantle, in particular, the uppermost and lowermost parts. In
addition to the Earth, there is a similar possibility that Mars’ mantle also possesses this kind of
remarkable viscosity contrast from the perspectives of the astrometrically-obtained tidal dissipation
and also the numerical simulation of the mantle convection with the influence of water inclusion.
Nevertheless, in the past, viscosity structure has been roughly averaged, and therefore, regarded to
include no mechanically-specific layer.
If a mantle possesses a low-viscosity layer, this layer is considered to greatly affect time evolution of
true polar wander. This is mainly because such a soft layer is expected to practically behave as a fluid
layer in response to centrifugal potential on a sufficiently long period of time. This response changes
intensity factors and characteristic time scales of relaxation modes of viscoelastic deformation. This
fact further means that the fluid-like response in this layer leads to a change in a time scale of
viscous readjustment of a hydrostatic shape on a planetary body. In consequence, a time length to
reach a state of rotational equilibrium depends on presence/absence of such a low-viscosity layer,
and if present, on its depth as well. This sort of dependence has never been discussed in the previous
approaches.
It would be important to understand this effect in order to quantitatively discuss theoretical validity
of true polar wander scenarios derived from observables, especially their time variations. Moreover,
useful information to constrain ancient viscosity structure is possibly available through a physical
condition as a cause of this phenomenon.
In this study, model calculation on long-term polar motion accompanied by viscoelastic deformation
are performed in order to investigate the effect of a low-viscosity layer inside a mantle of a solid
planetary body on a time scale of true polar wander. Here a planetary body is supposed to be similar
to the Earth or Mars, but with the low-viscosity zone. The most important key is dependence of the
viscoelastic response on this low-viscosity layer. On the other hand, note that deformation process in
here is regarded to be incompressible for solving normal modes of viscoelastic Love numbers. For
the sake of the calculation based on this assumption, the interior structure is still simplified to some
extent except for the presence of the low-viscosity zone. However, this simplification does not affect
the validity of the subsequent discussion.
In this calculation, the quasi-fluid approximation is applied so that the polar motion equation can be
integrated just as a nonlinear one. The reason is that the linear approximation is not generally
applicable to large polar motion of a magnitude of several tens of degrees as discussed here.
Following the application limit of the quasi-fluid equation, load formation is assumed to be much
slower than characteristic time scales of viscoelastic deformation. This approximation scheme has
already been constructed by the author as well as some other researchers. The present study also
deals with this integration in the same manner.
As a result, the above calculation indicates the fact that the time variation of a spin pole with the
effect of the low-viscosity layer is faster compared to that without it. In addition, the result also
reveals that, the shallower the low-viscosity zone is, the faster the polar wander speed is. The reason
why the low-viscosity layer makes polar wander speed faster is because the behavior of this layer is
like that of liquid even with respect to relatively short-term variation of external forcing. This
corresponds to, in turn, faster hydrostatic readjustment to centrifugal potential perturbation, which
shortens a time scale of variation in the moment of inertia tensor associated with that in the spin axis.
Furthermore, variation of an oblate shape with viscous relaxation of this layer negatively depends on
the thickness of the upper shell which elastically reduces the above-mentioned fluid-like
displacement of the layer. This point assures that the effect of the low-viscosity layer on polar
wandering is stronger if the upper shell is thinner, that is, this soft layer is shallower.
The calculation result shown above provides the conclusion that the presence of the low-viscosity
layer in a planetary interior largely affects true polar wander even if the layer is relatively thin. The
previous studies simplified mantle viscosity structure and ignored the low-viscosity layer inside.
Unlike them, the present study demonstrates time evolution of true polar wander with the explicit
effect of this specific layer. Although it has been pointed out in the past that such an easily
deformable domain plays an important role in viscoelastic deformation induced by tide or load on the
Earth, this point is the same in the case of secular rotational motion.
It should be noted, however, that the present calculation is also based on the assumption of
incompressibility like the former one. Possible effect of compressibility might be required for more
realistic calculation in the future.
Lunar Global Iron Mapping with Partial Least Squares Regression
Lingzhi Sun, Zongcheng Ling
School of Space Science and Physics and Shandong Provincial Key Laboratory of Optical As- tronomy &
Solar-Terrestrial Environment, Shandong University, Weihai, Shandong 264209, P. R. China
Introduction: Knowledge of lunar iron distribution will lead to a better understanding of the lunar
nature and petrogenesis[Ling, 2011;Taylor,1987]. There are many algorithms derived to estimate
lunar iron abundance from Clementine UVVIS images [Lucey 1995;Blewett,1997;Lucey
1998;Lucey,2000;Gillis 2004]. In this paper, we choose to modeling the FeO distribution with Partial
Least Squares Regression (PLS) method. PLS has been regarded as the second generation of
regression methods, which can perform well in multivariable regression especially when there exists
multiple correlation among variables. Here we present a model derived from Clementine UVVIS
images, which performs well in estimating lunar iron abundance as well as suppressing the space
weathering effect of lunar surface. We applied this model to Clementine UVVIS global data sets and
derived a lunar global iron map, then compared our result with previous FeO algorithms and those
measured by Lunar Prospector (LP) neutron spectrometers.
PLS Modeling: We aim to find the statistical correlations between reflectance data and iron
abundance for lunar surface, and suppress the maturity effect at the same time. We took the
reflectance spectra as our independent variable, and then derived effective absorbance by applying
a natural logarithmic function to each reflectance data before modeling. The absorbance is assumed
to have a linear relation to the abundance of a constituent [Li 2006]. Iron contents and optical
maturity index were taken as induced variable, and they were orthogonalized in the regression in
order to avoid interior correlation.
First, Clementine UVVIS images of the lunar sample-return sites are processed and used to
build the PLS model, the maturity index is computed with the parameters presented by Lucey 2000a
[Blewett 1997;Lucey 2000a,b;Wilcox,2005]. Then we get Model-1, and apply it to an area near the
southern rim of Mare Crisium to derive iron map (Fig.1 b). Comparing to Lucey’s method[Lucey
2000], the maturity suppress is unclear, cause the iron content in fresh craters are higher than its
neighboring area. For statistical result, the bimodal distribution presented in Fig.2 is related to lunar
highland and mare regions. Model-1’s iron content (Fig.2 b) is a little higher in highland area and
lower in mare area comparing to Lucey’s result (Fig.2 a).
Then the limitation of sample-return data is recognized and we notice that modeling with
statistical regression methods highly rely on the sample data. Then we select some more spectra
around the sampling sites, iron and optical maturity (OMAT) content are calculated with Lucey’s
parameters [Lucey 2000]. While selecting data, we try to find the data represent different iron
content and space weathering effects, i.e., those locations ranging from very low to very high iron
content as well as those from very mature to very immature. With our sample-return data, selected
data as well as data from lunar far side into modeling data, we built Model-2, and the iron map is
shown in Fig.1 c.
Our result shares a lot of similarities with Lucey’s algorithm. The average iron content is very
close between our result and Lucey’s algorithm (Lucey’s result is 15.19 wt.%, Model-2’s result is
15.20 wt.%). As is shown in Fig.2 c, for major mare soils iron content, our modeling result is almost
the same with Lucey’s (16 wt.%).However, our result seems to present a higher iron content (9 wt.%)
in high-land region comparing to Lucey’s algorithm (8 wt.%). iron map derived from Model-2 also
performs well in maturity suppressing, regions with fresh craters distributed looks like uniform in
iron content. As shown by statistical result (Fig.3), for average OMAT value, our result (0.147) is a
little higher when comparing to Lucey’s (0.151). Lucey’s OMAT is bimodal distributed, which
indicate that the maturity effect in their result hasn’t been completely removed from iron distribution.
However, this bimodal distribution of OMAT is not shown in our result, which can be seen from
Fig.3.
The discrepancies of highland iron content between Lucey’s algorithm and Model-2 may be
from the difference of method. We choose PLS modeling with all the five bands in Clementine
images to derive iron map, while only two bands (B2:750nm, B4:950nm) are concerned in Lucey’s
band ratio method.
Fig.1 Left: Clementine UVVIS image(750nm), reflectance are very high in fresh craters ; Right:
Comparison of iron map among Lucey’s algorithm(a), Model-1(b) and Model-2(c)
Fig.2 Statistical result of iron map from Lucey’s algorithm(a), Model-1(b) and Model-2(c)
Fig.3 Statistical results of OMAT, red: OMAT calculated from Lucey 2000, a little peak can be seen
where OMAT value is between 0.117 and 0.125; Blue: OMAT calculated from Model-2
Global iron mapping：We apply Model-2 into clementine UVVIS image (resolution: 1km/pixel)
[http://ser.sese.asu.edu/MOON/clem_color.html], and derive global iron map (as is shown in Fig.4).
For average iron content, there are little difference between Lucey’s result (7.8 wt.%) and our (7.9
wt.%), but our result is a little higher in global mode (our result is 5.5 wt.%, Lucey’s result is 4.7
wt.%). Lunar prospector (LP) has obtained a global iron map using a neutron spectrometer, which
shows the global mode is 6.4 wt.%. Our iron map agree with that derived from LP.
Lucey et al. has derived a global iron map using Clementine image in 1995, and their work
pronounced to support the lunar magma ocean hypothesis [Lucey 1995]. While the spectra data they
used was directional-hemispherical laboratory spectra, which will introduce error while applying to
bidirectional spectra data. Lucey et al. modified their model by resolving lunar sample stations with
Clementine images, and the global mode from their new iron map was 4.5 wt.% .Korotev et al. noted
that the feldspathic lunar meteorites have iron ranging from 4.3 to 6.1 wt.%. Our new FeO
predictions of lunar farside are within in the laboratory measured values from lunar meteorites.
Fig.4 Global iron mapping using Clementine UVVIS image
Conclusions: We have derived a clementine global iron map using PLS method, and our work
agrees with former lunar iron studies. Our result is also supported by LP iron measurements and
lunar meteorite studies.
A new lunar global DEM derived from Chang’E-1 Laser Altimeter
data with crossover adjustment
Kaichang Di, Wenmin Hu, Zhaoqin Liu
State Key Laboratory of Remote Sensing Science, Institute of Remote Sensing and Digital Earth, Chinese Academy
of Sciences, Beijing 100101, P.R. China
Abstract: This paper presents a new lunar global digital elevation model (DEM) derived from
Chang'E-1 Laser Altimeter (LAM) data based on crossover adjustment with local topographic
constraint. With about 9.12 million altimetric points acquired by the LAM, we derived more than
141,000 crossovers that cover the entire lunar surface after eliminating outliers of orbits and
altimetric points. The height differences at the crossovers represent the LAM data errors caused by
many factors. To reduce the errors, the global lunar surface is divided into 32 local blocks, and the
least squares adjustment of crossover differences is performed for each block using the local
topographic constraint information extracted from the planar areas. Smooth transitions among the
neighbouring blocks are ensured through sufficient overlapping areas and virtual control points from
the planar areas. After the crossover adjustment, root mean square (RMS) of the residuals is reduced
from 149.51 m to 54.75 m after using three parameters for each profile in each block in the
mid-latitude region. In polar regions, RMS is reduced from more than 150 m to less than 100 m after
using seven parameters for each profile. The resulting lunar global DEM has a significantly
improved quality in the local consistencies, i.e., artifacts in the original DEM are eliminated or
decreased. The new lunar global DEM is also compared with the laser altimeter data from NASA’s
LRO mission and JAXA’s KAGUYA mission. After comparison, the result shows that the DEMs are
consistent and that adjustment does not deform the lunar terrain.
Multiple Image Shape-From-Shading for Detailed Lunar Terrain
Mapping Using Chang’E Images
M. Peng , K. Di, Y. Liu
State Key Laboratory of Remote Sensing Science, Institute of Remote Sensing and Digital Earth, Chinese Academy
Sciences, Beijing, China 100101.
Abstract: China's Chang'E project has obtained orbital images covering the entire lunar surface.
Precision lunar terrain mapping is critical for the follow up landing and rover exploration and
scientific research. The traditional photogrammetric mapping method usually can't provide
pixel-level detailed mapping products effectively. In the paper we propose a new multiple image
Shape-From-Shading (SFS) method for detailed lunar terrain mapping that incorporates line sensor
geometry and photometry models. Based on the SFS principle and an initial DEM derived from
stereo images, the lunar surface is segmented into regions with constant albedo and variable albedos.
A combined adjustment model is established based on linearized collinearity equations, interior
orientation model and lunar-lambert functions. Then, a least squares solution is adopted to achieve a
pixel-level 3D reconstruction of the lunar terrain. The new method is tested using lunar orbital
images acquired by Chang’E-1 and Chang’E-2 CCD sensors in the Sinus Iridum area. Experimental
results demonstrate that the developed multiple image SFS method is able to produce pixel-level
lunar terrain models precisely.
One possible origin of olivine in Copernicus crater: the remnants of
projectile
Z. Yue 1,2
, B. C. Johnson 3, D. A. Minton
2, H. J. Melosh
1, 2, K. Di
1, W. Hu
1, Y. Liu
1
1 State Key Laboratory of Remote Sensing Science, Institute of Remote Sensing and Digital Earth, Chinese
Academy Sciences, Beijing, China 100101. 2 Department of Earth, Atmospheric and Planetary Sciences, Purdue University, West Lafayette, Indiana, USA
47907. 3 Department of Physics, Purdue University, West Lafayette, Indiana, USA 47907.
Abstract: The mineral olivine has been found in the central peaks of Copernicus crater and usually
interpreted as excavated from deep lunar crust or even mantle. In the paper we studied the formation
of Copernicus crater through hydrocode simulation and proposed that the olivine was more possible
from the projectile remnant than from the deep. In the simulation the target is modeled with four
layers of basalt, upper and lower lunar crust by granite, and lunar mantle by dunite from top to down.
Our simulation results show that the maximum excavation depth among the simulations is no more
than 7 km which is too shallow to reach the lunar mantle, while a large fraction of the projectile can
survive and sweep back in the crater center provided that the impact velocity is less than 12 km/sec.
To further validate the results, we also simulated the orbital evolution of the asteroids in the main
belt and derived that about 30% of lunar impacts occur at speeds below 12 km/sec. This finding has
great importance in interpreting the occurrence of olivine in other complex craters, including on
Moon and other terrestrial planets.
An approach based on shadow areas matching for visual navigation in
planetary landing
Wei Ruoyan, Ruan Xiaogang, Li Jiangeng
School of Electronic Information and Control Engineering，Beijing University of Technology，Beijing100124, China
Abstract: For the problem of landmark match to visual autonomous navigation in planetary landing
this paper provides an approach of planet surface’s shadow areas detection and affine matching
between descent images for attitude, motion, local location estimation and hazard avoidance, which
can improve the precise of landing. The approach can maintain the features matching rate at a high
level between descent images even the attitude difference of the images is large and with no attitude
measurements supply. First, a new method is proposed to extract the planet surface’s shadow areas as
the landmarks. Then an affine normalization algorithm is applied to normalize the areas, and an
Awsift descriptor is proposed for matching the normalization shadow areas between two consecutive
descent images. Series of experiments show that when the images have some viewpoint
transformation the result can still reach a certain high matching rate. For rectification the mismatches
a method is proposed for estimating the parameters of affine transformation in the matching result
which mixed with correct and incorrect matched pairs. Finally, real sequence images of 433 Eros are
utilized to test the performance of the approach and the results show that the proposed approach is
able to match the required number of shadow areas without false matching.
Key words: Shadow areas matching; Affine normalization; Mismatch rectification; Visual
autonomous navigation
Landing area terrain reconstruction method combined laser
rangefinder
Qunshan Shi1, Qing Xu
1, Chaozhen Lan
1 , Jiansheng Li
1 Zhengzhou Institute of Surveying and Mapping
Zhengzhou, China;
Abstract: How to reconstruct terrain using the sequence images and laser altimeter data when the
detector is vertically descending is researched. A new topographic reconstruction method of the
landing area of the detector is proposed combined laser data and image sequence by the optical
navigation camera. Using relationship between the object height difference and the vertical descent
movement characteristics of the detector, a new terrain reconstruction mathematical model is
deduced. The influence of the detector attitude jitter on solver model is considered, and a solution is
given. Because the accuracy of the model is affected by the image noise, the solver model is
presented when the image nose exists. Finally, this terrain reconstruction method is validated by
mathematical simulation, results show that the method can meet terrain reconstruction precision
requirements, which can provide data support for high-precision soft landing.
Key Words: Landed detection; descending image; Laser Ranging; terrain reconstruction;
New estimate of the present Earth expansion based on geodetic
observations
Wen-Bin Shen1,2*
, Zi-Yu Shen 1
, Rong Sun 1
1 School of Geodesy and Geomatics/Key Laboratory of the Geospace Environment and Geodesy, Wuhan
University, Wuhan 430079, China 2 State Key Laboratory for Information Engineering in Surveying, Mapping and Remote Sensing, Wuhan
University, Wuhan 430079, China
*Correspondence: [email protected]
Abstract: Precise estimate of Earth expansion may provide better understanding of the Earth
evolution and its structure. This study further investigates an earlier study of Shen et al 2011, which
suggests that the Earth is expanding at a rate about 0.2 mm/yr at present based on the temporal
principal inertia moments of the Earth and the average vertical variations of more than 800 stations
on ground. Observations by satellite altimetry measurements show that the average sea level rise
(SLR) is about 3.3 mm/yr in recent years (Nicholls et al 2010). Taking into account the total
contributions to the SLR due to glacier and ice sheet melting (1.49 mm/yr, Jacob et al. 2012), global
temperature increase (1.03 mm/yr, which coincide well with the result 0.9 mm/yr of WOA09) and
post-glacier respond (PGR) effects (-0.24 mm/yr), we find that the ocean bottom is expanding in
average at a rate around 1.0 mm/yr in recent twenty years. Since a relative large uncertainty exists,
which is due to the fact that the sea level rise and the relevant contributions to it cannot be well
estimated at present, we need further investigations to precisely estimate of the Earth expansion.
However, the estimate of a weighted result of the Earth expansion is about 0.2 mm/yr at present. This
work was supported by the Natural Science Foundation of China (grant No. 41174011), National 973
Program China (grant No. 2013CB733305), Funds for Creative Research Groups of NSFC (grant No.
41021061), and NSFC (grant Nos. 41128003, 41210006, 40637034).
Key Words: Earth expansion; space-geodetic data; gravimetric data; sea level rise
Analysis on lunar thermal infrared emissivity spectral features:
application to the Diviner Lunar Radiometer data
Ma Ming, Chen Sheng-bo, Lian Yi, Guo Peng-ju
College of Geoexploration Science and Technology, Jilin University, Changchun 130026
Email:[email protected]
Abstract：Thermal infrared emissivity spectra of Lunar Soils have diagnostic features that could
indicate rock and mineral compositions, mainly including the Christiansen Feature (CF), the
Reststrahlen Bands (RB) and the Transparency Feature (TF). In this study, the relationship between
different spectral features and mineral physical properties (i.e., maturity, particle size, mineral
composition and chemical composition) is established by using 16 reflectance spectra of lunar soils
derived from Reflectance Experiment Laboratory (RELAB). These reflectance (R) spectra can be
used to calculate absolute emissivity (E) using Kirchhoff’s Law (E=1-R). The Christiansen Feature
can be related to the composition, temperature and surface condition without being much affected by
particle size and maturity. The CF position is closely correlated to the sample’s bulk FeO abundance,
with a Pearson Correlation Coefficient (r) of 0.9. As for Reststrahlen Bands, absorption positions,
shapes and intensities, and the amount of absorptions are dependent on the composition and particle
size. The abundance of Plagioclase, Pyroxene and Olivine determine the Reststrahlen Bands
absorption positions and shapes, while particle size determines intensities. Among the three spectral
features, TF has a minor influence and is not identifiable on the moon, and that is why the
relationship is usually neglected. Then we apply the relationship between physical property and
spectra features to inverse new thermal infrared data sets, including the Diviner Lunar Radiometer
Experiment on the Lunar Reconnaissance Orbiter.
Key words: Lunar Soils; Emissivity spectra; The Christiansen Feature; the Reststrahlen Bands;
Diviner
Table 1. Is/FeO (Maturity), CF Values (mm) Derived From RELAB Spectra, Published FeO and TiO2
Abundances (wt. %) for 5 Lunar Soils (20–45 mm Size Fractions) As Well As Pyroclastic Glasses 74002 and
15401 (Bulk Samples)
Apollo Sample Is/FeO CF FeO TiO2
11 10084 78 8.39 15.5 8.30
12 12001 56 8.35 16.9 3.20
15 15041 94 8.31 15.2 2.03
16 61141 76 8.19 5.2 0.58
17 70181 53 8.42 16.0 8.11
17 74002 <1 8.63 22.7 9.2
15 15401 6 8.39 16.3 1.08
2 4 6 8 10 12 14
0.5
0.6
0.7
0.8
0.9
1
Wavelength(um)
Em
issiv
ity
12030
14141
61221
71061
Fig.1 thermal infrared emissivity spectra of 12030, 14141, 61221, 71061
2 4 6 8 10 12 14
0.5
0.6
0.7
0.8
0.9
1
Wavelength(um)
Em
issiv
ity
10084
67461
67481
71501
Fig.2 hermal infrared emissivity spectra of 10084, 67461, 67481, 71501
Table 2. Is/FeO (Maturity), Lunar soil smineral abundance for 12030, 14141, 61221, 71061, 10084, 67461,
67481, 71501
Soils 12030 14141 61221 71061 10084 67461 67481 71501
Is/FeO 14 5.7 9.2 14 78 25 31 35
Ilmenite 2.6 1.9 0.6 10.4 6.4 0.3 0.1 12.3
Plagioclase 15.3 26.8 58.7 13.9 16.8 64.3 61.2 16.5
Pyroxene 33.8 19.8 7.4 20.8 16 7.3 6.6 21.3
Olivine 4.3 4.0 3.9 3.9 1.4 2.5 4.0 3.6
Agglutinitic Glass 39.4 41.0 28.9 31.4 53.9 25.4 27.6 38.3
Volcanic Glass 1.2 4.5 0.2 18.9 3.4 0.1 0.3 6.7
Others 3.4 2.2 0.3 0.7 2.1 0.1 0.2 1.3
Total 100 100 100 100 100 100 100 100
2 4 6 8 10 12 14
0.5
0.6
0.7
0.8
0.9
1
Wavelength(um)
Em
issiv
ity
Bulk Particulate
0-25um (Dry sieved)
0-25um (Wet sieved)
25-45um (Wet sieved)
45-75um (Wet sieved)
Fig.3 thermal infrared emissivity spectra of different particle size (67627)
MERTIS on BepiColombo - seeing Mercury in a new light
Jorn HELBERT1#+
, Mario D'AMORE1, Alessandro MATURILLI
1, Ingo WALTER
1, Gisbert PETER
1,
Thomas SÄUBERLICH1, Harald HIESINGER
2
1DLR, Germany,
2Wilhelms Universität Münster, Germany
#Corresponding author: [email protected]
+Presenter
The MErcury Radiometer and Thermal infrared Imaging Spectrometer (MERTIS) is part of the
payload of the Mercury Planetary Orbiter spacecraft of the ESA-JAXA BepiColombo mission. The
mission is scheduled for launch in 2015 with arrival at Mercury in 2021.
MERTIS’s scientific goals are to infer rock-forming minerals, to map surface composition, and to
study surface temperature variations on Mercury with an uncooled microbolometer detector. In order
to achieve these goals MERTIS will map the whole surface of Mercury with a spatial resolution of
500m for the spectrometer channel and 2km for the radiometer channel. The MERTIS dataset is
unique. None of the instruments on the NASA MESSENGER mission currently in orbit around
Mercury covers the same spectral range or provides a measurement of the surface temperature. The
MERTIS will complement the results of MESSENGER as well as those of the other instruments on
BepiColombo. MERTIS will for example be able to provide spatially resolved compositional
information on the hollows and pyroclastic deposits – both among the most exciting discoveries by
the MESSENGER mission.
MERTIS combines a push-broom grating thermal infrared spectrometer with a thermal infrared
radiometer that share the same optics, instrument electronics, and in-fight calibration components
and span wavelength ranges of 7-14 and 7-40 µm, respectively. MERTIS combines several new
approaches. The spectrometer channel uses an uncooled microbolometer as detector and a
micro-machined grating which in combination achieve a spectral resolution better then 200nm with a
signal to noise ratio of up to 400 for the highest surface temperatures. The radiometer channel is
integrated in the slit of the spectrometer allowing using the same optics and the same calibration
sources for both channels. This highly integrated design allowed keeping the instrument mass at
3.3kg with an average power consumption of 12W.
Joint GNSS and SLR Data for the Study of Earth Rotation Parameters
WEI Erhu1,2
, WAN Lihua1
(1 School of Geodesy and Geomatics, Wuhan University, 129 Luoyu Road, Wuhan 430079,
China)
(2 Key Laboratory of Geospace Environment and Geodesy, Ministry of Education, Wuhan
University, 129 Luoyu Road, Wuhan 430079, China)
Abstract: ERP (Earth Rotation Parameters) means the parameters of the change of the Earth rotation
speed (UT1-UTC) and polar coordinates(xp,yp). Currently, IERS (International Earth Rotation
Service Organization) and data processing centers of IGS (International GNSS Service) are involved
in the maintenance of the global coordinate reference system and release of the Earth rotation
parameters. IERS use LLR, SLR, VLBI, Doris and GPS measures and calculates parameters of the
Earth rotation which has reached the accuracy of subcentimeter, an ERP solution per day.
SLR, VLBI technology has the characteristics of high-precision in determination of the Earth
rotation parameters. however, the lack of observational data makes it only give one solution per day
which can’t meet the requirements of high rate; GNSS technical computing accuracy is not as good
as SLR, VLBI, but the large number of observation data make it possible to use observation of 1 o 2
hours to solve Earth orientation parameters. Joint SLR and GNSS data to solve the ERP parameter
will satisfy both the requirements of high precision and high temporal resolution.
This paper mainly does the following work:
(1) introducing GNSS and SLR space technology and the principles of measuring the Earth's rotation
parameters;
(2) selecting appropriate GNSS observations and SLR observations to get ERP solution, respectively,
then analysing the related accuracy by comparing the results with IGS;
(3) introducing combined ERP parameters solver methods of GNSS and SLR and then analysing the
precision of combined results of GNSS and SLR;
(4) the high temporal resolution of the ERP parameters that measuring by only GNSS and the
integrated solution may exists system deviation, the article has used parameter conversion method to
eliminate the bias and then analysed the results.
Key words: GNSS; Earth rotation parameters; SLR; joint solution; ERP
Long-term forecasts of polar motion based on LS_AR model
WEI Erhu1,2
, YANG Yali1
(1 School of Geodesy and Geomatics, Wuhan University, 129 Luoyu Road, Wuhan 430079,
China)
(2 Key Laboratory of Geospace Environment and Geodesy, Ministry of Education, Wuhan
University, 129 Luoyu Road, Wuhan 430079, China)
Abstract: Earth orientation parameters are made of the polar motion, day-to-day variations, nutation
and precession, which constitute a description of the parameters of the Earth's rotation changes,
called as ERP. ERP provides evidence for the relationship between the earth-fixed coordinate system
and instantaneous celestial coordinate system, the polar motion parameter as one of the orientation
parameters of the Earth, has a very important role in the celestial coordinate system and the Earth
coordinate system conversion, but also for orbit determination, deep space geodesy, satellite
navigation, etc., In this fields, polar motion play an indispensable function. Earth Orientation
Parameters geodynamics also contains a wealth of information. Researching polar motion parameter
is also important for the development of geophysics
Polar motion parameters are always provided by Organization IERS, IVS, etc. Forecasting polar
motion parameter by least squares extrapolation and model GM (1,1) model and artificial neural
network model, and the assembly of models. But the researches in this field are always focusing on
the short-term forecasting, so the article focuses on the long-term forecasting which are rarely
involved in study with analysis and modeling. Then the article tests the model with the data of polar
motion parameter time-series coming from the IERS.
In this paper:
(1) I study and analyze the constitution and establishment of the least-squares extrapolation model
(LS) and the regression model (AR) model, as well as the combination of the two and complete it by
programming.
(2) The article work on the problem by studying the changes in model building factor that may
change the model prediction accuracy and changing the method for establishing LS_AR model to
explore these changes polar motion parameters for the impact of long-term forecast accuracy by
forecasting analysis, accuracy evaluation, and the most suitable impact factor models and analyzed.
The composition of items on LS_AR model and implementation for analysis may affect the
long-term forecast of the polar motion changes, so the article makes the design for comparison.
This long-term focus is to make sure whether the original forecast model should be changed or
should not be changed, with comparison of changing the program or not and further analysis of
factors affecting long-term forecasts, I tend to arrive at an optimal design plan for everyone to refer.
Key words: polar motion; LS_AR model；mid-and-long term forecasting
Topographic Correction based Retrieval of Lunar Clinopyroxene
Abundance from M3 Data
Guo Peng-ju,Chen Sheng-bo,Wang Ming-chang,Wang Jing-ran,Li Yan-qiu
(College of Geoexploration Science and Technology,
Jilin University, Changchun 130026)
Email:[email protected]
Abstract：Lunar mineral has directly recorded the early evolution of lunar crust and the following
geological processes acting on it. However, in mountainous region, remote sensing data vary with
slope, aspect and surrounding terrain, which need to be considered before mineral abundance
inversion. In this paper, considering there is no atmosphere on the moon and sky diffuse irradiance is
ignored, the irradiance received by the target is divided into solar direct irradiance and adjacent
terrain-reflected irradiance. In order to calculate these irradiances, Sandmeier model is employed for
topographical correction to lunar surface reflectance. Because the moon is not a lambert reflector,
directional-directional reflectance and hemispheric-directional reflectance are introduced in the
model, which are used to calculate lunar flat surface directional-directional reflectance. When no
considering backscatter, Hapke models respectively applied in the satellite and lab measurement are
used to calculate the lunar surface albedo from the topographic corrected reflectance for Moon
Mineralogy Mapper(M3) data obtained by Chandrayaan-1 satellite. Spectral mixing analysis (SMA)
is then applied to the spectra unmixing of lunar surface albedo to retrieve the clinopyroxene
abundance in Sinus Iridum. The reflectance and clinopyroxene abundance retrieved are compared
with non-topographic correction results. And the topographic corrected based clinopyroxene
abundances retrieved are much faithful by comparing it with known Apollo 16 samples.
Key words: Topographic correct; Sandmeier model; Lunar mineral abundance; Hapke model; Sinus
Iridum; M3
data
Longitude (°)
Lati
tud
e (
°)
-37.820 -35.970
48.310
46.728
45.146
43.564
41.982
40.400
0.02
0.04
0.06
0.08
0.1
0.12
0.14
0.16
0.18
Reflectance
Longitude (°)
Lati
tud
e (
°)
-37.820 -35.970
48.310
46.728
45.146
43.564
41.982
40.400
0.02
0.04
0.06
0.08
0.1
0.12
0.14
0.16
0.18
Reflectance
(a) (b)
Fig.1 Reflectance of Sinus Iridium edge before (a)and after(b) topographic correction
Fig.2 Location of selected pixels of sunny slope a and shady slpoe b
(a) (b)
Fig.3 Reflectance of sunny slope(a) and shady slope(b)before and after correction
Longitude (°)
Lat
itu
de
(°)
-37.820 -35.970
48.310
46.728
45.146
43.564
41.982
40.400
0.05
0.1
0.15
0.2
0.25
0.3
0.35
0.4
0.45
0.5
Clinopyroxene
Longitude (°)
Lat
itu
de
(°)
-37.820 -35.970
48.310
46.728
45.146
43.564
41.982
40.400 0
0.05
0.1
0.15
0.2
0.25
0.3
0.35
0.4
0.45
0.5
Clinopyroxene
Fig.4 Clinopyroxene abundance of Sinus Iridium edge
before(a) and after(b) topographic correction
460.99 910.14 1249.50 1618.80 2297.50 2976.200.01
0.02
0.03
0.04
0.05
0.06
0.07
Wavelength (nm)
Ref
lect
ance
Shady slope before correction
Shady slope after correction
460.99 910.14 1249.50 1618.80 2297.50 2976.200.01
0.02
0.03
0.04
0.05
0.06
0.07
Wavelength (nm)
Ref
lect
ance
Sunny slope before correction
Sunny slope after correction
Longitude (°)
Lati
tud
e (
°)
13.869 16.681
-5.336
-6.816
-8.296
-9.776
-11.256
-12.736
0.01
0.02
0.03
0.04
0.05
0.06
0.07
0.08
0.09
0.1
Clinopyroxene
Fig.5 Result of topographic corrected based clinopyroxene abundance retrieved of Apollo16
Table 1. Comparison of calculated and measured abundance
of clinopyroxene from Apollo 16
method abundance
average of spectral mixing analysis 0.009
average of measured 0.014
4. Participants List
NO. NAME AFFILIATION COUNTRY EMAIL
1 Nader Haghighipour Univ. of Hawaii-Manoa USA naderh(at)hawaii.edu
2 Yansong Xue SHAO, CAS China xys(at)shao.ac.cn
3 Kanako Seki Nagoya University Japan seki(at)stelab.nagoya-u.ac.jp
4 Tengyu Zhang SHAO, CAS China zhangty(at)shao.ac.cn
5 Mau C. Wong JPL, NASA USA mau.c.wong()jpl.nasa.gov
6 Kwing Lam Chan HK Univ. Sci. Tech. Hong Kong,
China maklchan(at)ust.hk
7 Xuechuan Li SHAO/WHU China leexc0124(at)163.com
8 Roger Yelle Univ. Arizona USA yelle(at)lpl.arizona.edu
9 Alexander Gusev Kazan Univ. Russia alexander.gusev(at)mail.ru
10 Kaichang Di Int. RS. Dig. Earth, CAS China kcdi(at)irsa.ac.cn
11 Maria Teresa Capria INAF Italy mariateresa.capria(at)iaps.inaf.it
12 Susan
Mckenna-Lawlor Space Technology Ireland Ltd Ireland stil(at)nuim.ie
13 Mau C. Wong JPL, NASA USA mau.c.wong(at)jpl.nasa.gov
14 Wei Shao Qingdao Univ. of Sci. & Tech. China shaowei_qd(at)126.com
15 Vladimir Kontar Federal GEOS Funding, Inc. USA vkontar.geos(at)gmail.com
16 Shuanggen Jin SHAO, CAS China sgjin(at)shao.ac.cn
17 Paul Hartogh MPI for Solar System Res. Germany hartogh(at)mps.mpg.de
18 Taishan Lou BUAA, Beijing China tayzan(at)sina.com
19 Luciano Iess Uni. Roma Italy luciano.iess(at)uniroma1.it
20 Sun Kwok Uni. Hongkong China sunkwok(at)hku.hk
21 Athena Coustenis Paris Observatory France athena.coustenis(at)obspm.fr
22 Douglas N. Lin UC Santa Cruz USA lin(at)ucolick.org
23 Jinjin Zhao NAO, CAS China zhaojj(at)nao.cas.cn
24 Juergen Schmidt Univ. of Oulu Finland jrschmid(at)sun3.oulu.fi
25 Nishant Arora Inst. of Science & Technology India er.nishantarora192(at)gmail.com
26 Zongyu Yue Int. RS. Dig. Earth, CAS China yuezy(at)irsa.ac.cn
27 Koji Matsumoto NAOJ Japan koji.matsumoto(at)nao.ac.jp
28 Yuhui Zhao PMO, CAS China zhaoyuhui(at)pmo.ac.cn
29 Johanna Erika
Valdueza Univ. Philippines Diliman Philippines jevaldueza(at)gmail.com
30 Miriam Rengel MPI for Solar System Res. Germany rengel(at)mps.mpg.de
31 Yansong Xue SHAO, CAS China xys(at)shao.ac.cn
32 Wing-Huen IP National Central University Taiwan wingip(at)astro.ncu.edu.tw
33 Jianghui Ji PMO, CAS China jijh(at)pmo.ac.cn
34 G. Kochemasov IGEM, Russian Acad. of Sci. Russia kochem.36(at)mail.ru
35 Sahnggi Park ETRI South Korea sahnggi(at)etri.re.kr
36 Hauke Hussmann DLR Germany hauke.hussmann(at)dlr.de
37 Man Peng Int. RS. Dig. Earth, CAS China pengman(at)irsa.ac.cn
38 Sanjay Limaye Univ. of Wisconsin-Madison USA sanjayl(at)ssec.wisc.edu
39 Tomas Ignacio Gomez Universidad de Chile Chile tomas.ignacio.gomez(at)gmail.com
40 Long Xiao China Univ. Geosci. China longxiao(at)cug.edu.cn
41 Leonid Zotov Sternberg Astron. Institute Russia wolftempus(at)gmail.com
42 Varun Sheel PRL India varun(at)prl.res.in
43 Qunshan Shi Inst. Surveying and Mapping China hills1(at)163.com
44 Nader Haghighipour Univ. of Hawaii-Manoa USA naderh(at)hawaii.edu
45 Yao Dong PMO, CAS China dongyao(at)pmo.ac.cn
46 Luciano Iess Univ. of Rome Italy luciano.iess(at)uniroma1.it
47 Naveen Chandra Indian Ins. Tech. India naveenchandra0408(at)gmail.com
48 Yunlong Lin Univ. of California, Davis USA yunlong.frank.lin(at)gmail.com
49 Wojcieh Markiewicz MPI for Solar System Res. Germany markiewicz(at)mps.mpg.de
50 Qin Xu Inst. Surveying and Mapping China gengxun.rs(at)gmail.com
51 Xun Geng Inst. Surveying and Mapping China gengxun.rs(at)gmail.com
52 Chaozhen Lan Inst. Surveying and Mapping China gengxun.rs(at)gmail.com
53 Oliver Baur Space Res. Ins., AAS, Austria oliver.baur(at)oeaw.ac.at
54 Su Wang PMO, CAS China wangsu(at)pmo.ac.cn
55 Yunzhang Wu BUAA China wuyunzhang1982(at)126.com
56 Anil Bhardwaj Vikram Sarabhai Space Centre India Anil_Bhardwaj(at)vssc.gov.in
57 Kanako Seki Nagoya University Japan seki(at)stelab.nagoya-u.ac.jp
58 Zheng Xu Tech. Univ. of Delft Netherlands Z.Xu-1(at)tudelft.nl
59 Yuri Barkin Moscow State Univ. Russia barkin(at)inbox.ru
60 Ruoyan Wei Beijing Univ. Tech. China weiruoyan1984(at)163.com
61 Erhu Wei Wuhan Univ. China ehwei(at)sgg.whu.edu.cn
62 Yousi Wu Wuhan Univ. China 1500195848(at)qq.com
63 Erhu Wei Wuhan Univ. China ehwei(at)sgg.whu.edu.cn
64 Wenbin Shen Wuhan Univ. China wbshen(at)sgg.whu.edu.cn
65 Yuri Barkin Moscow State Univ. Russia barkin(at)inbox.ru
66 Robert Tenzer Wuhn Univ. China rtenzer(at)sgg.whu.edu.cn
67 Tilman Spohn DLR Germany tilman.spohn(at)dlr.de
68 Jianguo Yan Wuhn Univ. China jgyan(at)shao.ac.cn
69 Siddan Anbazhagan Periyar Univ. India anbu02(at)gmail.com
70 Victor Tejfel Fessenkov Astrophysical Institute Kazakhstan tejf(at)mail.ru
71 Robert Tenzer Wuhn Univ. China rtenzer(at)sgg.whu.edu.cn
72 Robert Tenzer Wuhn Univ. China rtenzer(at)sgg.whu.edu.cn
73 Yunzhang Wu BUAA China wuyunzhang1982(at)126.com
74 Dong Wang Inst. Surveying and Mapping China gengxun.rs(at)gmail.com
75 Yifan Hou Inst. Surveying and Mapping China gengxun.rs(at)gmail.com
76 Yu He Inst. Surveying and Mapping China hy_conference(at)163.com
77 Eleonora Ammannito INAF, Rome Italy eleonora.ammannito(at)iaps.inaf.it
78 Shangxin Liu Wuhan Univ. China shangxinliu(at)whu.edu.cn
79 Wanhong Hao Ins. of Tracking &
Telecommunication Tech. China haowanhong(at)bittt.cn
80 Leonid Zotov Moscow State Univ. Russia wolftempus(at)gmail.com
81 Ming Ma Jilin Univ. China 121303083(at)qq.com
82 Pengju Guo Jilin Univ. China guopj11(at)mails.jlu.edu.cn
83 Yanqiu Li Jilin Univ. China 972987544(at)qq.com
84 Lian Yi Jilin Univ. China fishlice(at)163.com
85 Junichi Watanabe NAOJ Japan jun.watanabe(at)nao.ac.jp
86 N. A. Chujkova Moscow State Univ. Russia nason(at)sai.msu.ru
87 Yuzhong Wu IHEP, CAS China yzwu(at)ihep.ac.cn
88 Robert Rankin University of Alberta Canada rrankin(at)ualberta.ca
89 Liyun Zhang Guangzhou Univ. China liy_zhang(at)hotmail.com
90 Erika Valdueza Univ. of Philippines-Diliman Philippines jevaldueza(at)gmail.com
91 Giuseppe Piccioni INAF, Rome Italy [email protected]
92 Xiaohua Fang Colorado Univ. USA xiaohua.fang(at)lasp.colorado.edu
93 Yuji Harada China Univ. Geosci. China harada(at)shao.ac.cn
94 Qian Huang China Univ. Geosci. China qianhuang.83(at)gmail.com
95 Yuji Harada China Univ. Geosci. China harada(at)shao.ac.cn
96 Qing Liang China Univ. Geosci. China qliang(at)cug.edu.cn
97 Oleg Titov Geosci. Australia Australia Oleg.Titov(at)ga.gov.au
98 Maodeng Li Ins. of Tracking &
Telecommunication Tech. China mdeng1985(at)gmail.com
99 Jilin Zhou Nanjing Wuhan China zhoujl(at)nju.edu.cn
100 Rui Zhang Shanghai Univ. China ysljzhangrui(at)qq.com
101 Marco Gregnanin Uni. Roma Italy marco.gregnanin(at)uniroma1.it
102 Bo Wu Hong Kong Polytechnic Univ. China bo.wu(at)polyu.edu.hk
103 Luyuan Xu Wuhan Univ. China luyuanxu(at)whu.edu.cn
104 Lingzhi Sun Shandong Uni. - Weihai China zcling(at)sdu.edu.cn
105 Zhuoxiao Wang Tsinghua Univ. China physics5mickey(at)gmail.com
106 Cong Xie Wuhan Univ. China xiecong(at)whu.edu.cn
107 Dong Chen Harbin Ins. of Tech. China cd_hit2010(at)163.com
108 Shuaiyi Shi China Univ. Geosci. China 1575323318(at)qq.com
109 Chao Wang East China Normal Univ. China wangchaoecnu(at)gmail.com
110 Stefano Colpani SHAO/DTU Denmark stefano.colpani(at)gmail.com
111 Xin Zhao Shanghai Univ./SHAO China 75305860(at)qq.com
112 Xuelin Tao Hefei Univ. Tech. China studylin(at)163.com
113 Miaohang Kang Wuhan Univ. China 1242319296(at)qq.com
114 Yi Yang Wuhan Univ. China qysyy111(at)whu.edu.cn
115 Fang Zou SHAO, CAS China fangz070720(at)gmail.com
116 Shuai Xing Inst. Surveying and Mapping China gengxun.rs(at)gmail.com
117 Li Liu Wuhan Univ. China 1538097252(atqq.com
118 Guiping Feng SHAO, CAS China gpfeng(at)shao.ac.cn
119 Rongrong Guo Wuhan Univ. China rongronggao0006(at)sina.cn
120 Wei Yu Hefei Univ. Tech. China abcyuweiabc(at)163.com
121 Nasser Najibi SHAO, CAS China nasser.najibi(at)yahoo.com
122 Feixiong Huang Wuhan Univ. China 348278020(at)qq.com
123 Bang Wu Wuhan Univ. China bluebell1000(at)foxmail.com
124 Xinggang Zhang SHAO, CAS China zhangxinggang(at)shao.ac.cn
125 Mengna Jia Wuhan Univ. China 1607090715(at)qq.com
126 Lu Xu Wuhan Univ. China saifuji(at)126.com
127 Cui Yuan Wuhan Univ. China 740395964(at)qq.com
128 Pin Zhang Wuhan Univ. China zpkb1555(at)qq.com
130 Xuyuan Wang China Univ. Geosci. China 1602024843(at)qq.com
131 Zhiqiang Li Wuhan Univ. China leeche.1990(at)gmail.com
132 Yang Zhou Shanghai Univ./SHAO China 371877915(at)qq.com
133 Liang Chang SHAO, CAS China lchang(at)shao.ac.cn
134 Ayman A. Hassan SHAO, CAS China hassan.ayman(at)shao.ac.cn
135 Rui Jin SHAO, CAS China ruijin(at)shao.ac.cn
136 Lingzhi Sun Shandong Uni. - Weihai China slz1990(at)aliyun.com
137 Yi Yu China Univ. Geosci. China yypolaris(at)yeah.net
138 Chuan Yang Wuhan Univ. China 1120675758(at)qq.com
139 Zhixiang Yin Wuhan Univ. China yinzhixiang0630(at)126.com
140 Yi Yang Wuhan Univ. China qysyy111(at)whu.edu.cn
141 Shuhua Ye SHAO, CAS China ysh(at)shao.ac.cn
142 Jiannan Zhao China Univ. Geosci. China schwaitser(at)126.com
143 Bin Lu USTC, Hefei China ac21b(at)mail.ustc.edu.cn
144 Xuecao Shi USTC, Hefei China shxuecao(at)mail.ustc.edu.cn
145 Wei Zhang Nanjing Univ. China tianxinzw(at)sina.cn
146 Wanqiu He Wuhan Univ. China sherryhwq(at)163.com
147 Cui Yuan Wuhan Univ. China 740395964(at)qq.com
148 Shangxin Liu Wuhan Univ. China shangxinliu(at)whu.edu.cn
149 Kaidi Peng Wuhan Univ. China pengkaidi007(at)foxmail.com
150 Luping Zhong Wuhan Univ. China 1071261229(at)qq.com
151 Wei Wu Wuhan Univ. China 1259654613(at)qq.com
152 Fei Chen China Univ. Geosci. China 826627595(at)qq.com
153 Junhai Li Wuhan Univ. China jhlee(at)whu.edu.cn
154 Binbin Liao Wuhan Univ. China 1040407093(at)qq.com
155 Wenqiang Zhang Wuhan Univ. China wqzhang(at)whu.edu.cn
156 Mu Lin Wuhan Univ. China mulin(at)whu.edu.cn
157 Zhongkui Shi China Univ. Geosci China 302861051(at)qq.com
158 Yun Xu China Univ. Geosci. China 394146079(at)qq.com
159 Xiuyuan Zhang China Univ. Geosci. China 280485958(at)qq.com
160 Wenjin Chen Wuhan Univ. China cwjwhu(at)whu.edu.cn
161 Chuanming Liu China Univ. Geosci. China 2lcm123(at)gmail.com
162 Ding Chen Nat. Space Res Center, CAS China ding(at)nssc.ac.cn
163 Jingwen Liu Yanshan Univ. China liujw_gis(at)163.com
164 Haitao Shang University of Minnesota USA shan0306(at)d.umn.edu
165 Zhen Wang XAO, CAS China wangzh(at)xao.ac.cn
166 Chengguang Xue Wuhan Univ. China chgxue(at)whu.edu.cn
167 Shuai Zhang Wuhan Univ. China 810074010(at)qq.com
168 Guangyu Gong Wuhan Univ. China 527914541(at)qq.com
169 Hong Lian Wuhan Univ. China alice.lian(at)qq.com
170 Hutao Cui Harbin Inst. Tech. China [email protected]
171 Wenbin Shen Wuhan Univ. China [email protected]
172 Wenjin Yang Wuhan Univ. China [email protected]
173 Sze-leung Cheung Hong Kong Univ. Hong Kong,
China [email protected]
174 Jörn Helbert DLR Germany [email protected]
175 Shengbo Chen Jilin, Univ. China [email protected]
176 Lihua Wan Wuhan Univ. China [email protected]
177 Wenjie Liu Wuhan Univ. China [email protected]
178 Yali Yang Wuhan Univ. China [email protected]
179 Misha Barkin Moscow State Univ. Russia [email protected]
180 Yue Liang Wuhan Univ. China [email protected]
181 Zhiguo Meng Jilin Univ. China [email protected]
182 Yunzhao Wu Nanjing Univ. China [email protected]
183 Zhihan Qian SHAO China [email protected]
Shanghai Astronomical Observatory, Chinese Academy of Sciences
80 Nandan Road, Shanghai 200030, China Website: http://www.shao.ac.cn
