Instrumentation from the Ground & Up Greg Card · Stratospheric Ballooning – SUNRISE & HIWIND...

Instrumentation from the Ground & Up

Greg Card

01-September-2015

GROUND BASED: ACOS - MK IV MLSO ACOS - CHIP MLSO ACOS - PICS MLSO ASP NSO, Sacramento Peak (DST) ATST/DKIST GOS Devel. AURA/NSO ChroTel KIS, Tenerife CoMP CoMP-M NSO, Sacramento Peak MLSO DLSP NSO, Sac Peak (DST) Low-L ECHO – MLSO MLSO ECHO – Tenerife IAC, Tenerife FPI Africa US Air Force, Ivory Coast, Africa FPI Antarctica NSF, Palmer Station FPI China Chinese Academy of Science FPI China II Univ. of Science and Technology of China FPI Korea Korean Polar Research Institute, Antarctica FPI Lab Test Bed, FPI Trailer, Marshall Field Site FPI Resolute NSF, Resolute Bay, Canada K-Coronagraph MLSO Laboratory Scattering, Na D HAO, Boulder POLIS KIS, Tenerife Prominence Magnetometer NSO, Sac Peak (Evans) SCD Slovakian Academy of Science, Slovakia SPINOR NSO, Sacramento Peak (DST) STARE & STARE II IAC, Tenerife GROUND BASED SUPPORT: CG-1 Lab Design & Light Feed Boulder DST Polarization Calibration NSO, Sacramento Peak (DST) Spar Guider System Boulder Spar Guider System MLSO CURRENT GROUND BASED IN DEVELOPMENT: COSMO-LC MLSO ChroMag MLSO ViSP AURA/NSO, Haleakala

TOTAL SOLAR ECLIPSES: 1991 Eclipse MLSO 1994 Eclipse Putre, Chile 1998 Eclipse Westpunt, Curacao SPACE BASED: METEOR/SEE EER Systems / NASA Wallops Spartan 201 WLC NASA/GSFC & Harvard CfA TIMED/SEE HAO/LASP/NASA SPACED BASED SUPPORT: Compact Coronagraph NASA/GSFC Laboratory Starshades CU/CASA, Boulder SDO / HMI – PCU NASA & Stanford University Solar-B / Hinode – GCU NASA & Lockheed (LMSAL) STEREO COR-1 Coronagraph NASA/GSFC SOUNDING ROCKETS: 8-Position Geneva Controller NASA sounding rocket 36.124, White Sands, NM STRAOSPHERIC BALLOONS: HIWIND NASA, Kiruna, Sweden SUNRISE – Test Flight NASA, MPS, KIS, IAC, INTA, GACE, IAA, Ft. Sumner, NM SUNRISE I NASA, MPS, KIS, IAC, INTA, GACE, IAA, Kiruna, Sweden SUNRISE II NASA, MPS, KIS, IAC, INTA, GACE, IAA, Kiruna, Sweden CURRENT STRATOSPHERIC BALLOONS: HIWIND Reflight NASA, McMurdo, Antarctica

~50 PROJECTS FROM 1988 TO PRESENT

chronograph

coronagraph

co·ro·na·graph /kəˈrōnəˌɡraf/ noun: coronagraph; plural noun: coronagraphs An instrument that blocks out light emitted by the sun's actual surface so that the corona can be observed.

Spartan 201 White Light Coronagraph

SPARTAN 201: Studying the Sun's Corona The SPARTAN 201 series is investigating the solar corona--the thin upper layers of the sun's atmosphere, which reach temperatures of about 2 million degrees Fahrenheit. Scientists hope to determine the mechanisms that cause the heating of the corona and the acceleration of the solar wind, which originates in the corona, and explain why the corona is so much hotter than the rest of the sun. The first three SPARTAN 201 flights have already advanced our understanding of the solar wind and its origin. SPARTAN 201-05 observations will be coordinated with observations made from the Solar and Heliospheric Observatory (SOHO) satellite, a cooperative mission of the European Space Agency (ESA) and NASA. The second and third missions were coordinated with the passage of the Ulysses spacecraft over the sun's south and north poles. SPARTAN 201 is equipped with two complementary telescopes that can measure these emissions from the sun's corona. The white light coronagraph (WLC), provided by the High-Altitude Observatory in Boulder, Colo., will measure the density of the electrons in the coronal white light. The ultraviolet coronal spectrometer (UVCS) from the Smithsonian Astrophysical Observatory at Harvard will measure the velocities, temperatures, and densities of the coronal plasmas. The SPARTAN project offers the scientific community an intermediate capability for conducting investigations in space between that afforded by small payloads that remain in the orbiter and larger satellites that orbit the Earth for long periods of time.









MissionMission Dates

(Spartan Deployed)

Spartan

Mission

Time

Flight

DesignationVehicle

Mission

Duration

Miles

Traveled

Number

of Orbits

Orbit

Altitude

Orbit

Inclination

Spartan 201-014/8/93 - 4/17/93

(4/11/93 - 4/13/93)43:24:27 STS-56

OV-103

Discovery9d 06:08:24 3,853,997 148 157 X 162 nm 57°

Spartan 201-029/9/94 - 9/20/94

(9/13/94 - 9/15/94)43:24:28 STS-64

OV-103

Discovery10d 22:49:57 4,500,000 176 140 X 145 nm 57°

Spartan 201-039/7/95 - 9/18/95

(9/8/95 - 9/10/95)43:30:00 STS-69

OV-105

Endeavour10d 20:28:55 4,500,000 171 190 nm 28.4°

Spartan 201-0411/19/97 - 12/5/97

(11/21/97 - 11/24/97)0:32:00 STS-87

OV-102

Columbia15d 16:35:01 6,500,000 252 150 nm 28.5°

Spartan 201-0510/29/98 - 11/7/98

(11/1/98 - 11/3/98)43:24:27 STS-95

OV-103

Endeavour8d 21:43:56 3,600,000 134 310 nm 28.5°

55d 15:46:13 22,953,997 881












Visit from John “Denny” Holt,

Flight Director and Bill Wagner, NASA HQ


Spartan 201 payload representatives were assigned to the Team 4, EVA Recovery Operations, under the leadership of Steve Smith. Johnson Space Center’s

Neutral Buoyancy Lab or “WETF”.







STARE's Piece of Sky

The STARE telescope took the majority of its initial exposures pointed at a 5.7 degree square within the constellation Auriga, the Charioteer. This field-of-view was chosen because it lies within the star-rich band of the Milky Way and transits the zenith around midnight during the observing season. Within this field-of-view, photometry has been done on over 24,000 stars. The images to the right shows (from top to bottom) the field superposed on a starmap of Auriga, the 5.7 degree square field as imaged by the telescope, and a 1.5 degree square blow-up of the field to show the multitude of stars detectable. Click on any to see a more detailed view.

http://www.hao.ucar.edu/research/stare/stare.html

STARE (STellar Astrophysics & Research on Exoplanets)



Stratospheric Ballooning – SUNRISE & HIWIND

A Near Space Experience: Long Duration Scientific Ballooning at

120,000 feet


SUNRISE: A Balloon-borne Solar Observatory SUNRISE is a balloon-borne solar observatory dedicated to the investigation of the key processes governing the physics of the magnetic field and the convective plasma flows in the lower solar atmosphere. These processes are crucial for our understanding of the magnetic activity of the Sun and of the outward transport of energy to heat its outer atmosphere and to fuel the eruptions and coronal mass ejections, i.e. phenomena that also affect the Earth system. SUNRISE is designed for operation in the stratosphere (at heights around 37 km) in order to avoid the image degradation due to turbulence in the lower terrestrial atmosphere and to gain access to the UV range down to 200 nm. Launched from above the polar circle at solstice conditions, SUNRISE enables an uninterrupted view at the Sun for extended periods of several days. This mission concept ideally combines the advantages of space-borne telescopes – undisturbed observations from above the atmosphere – with the advantages of ground based instrumentation. At a fraction of space mission costs the instrument can be recovered, refurbished or improved and reflown. The telescope with its aperture of one meter is the largest solar telescope to ever leave the ground. Equipped with inflight alignment and image stabilization it provides near diffraction-limited images for the highest spatial resolution of under 100 km on the solar surface.


Item Length [ft]

Balloon (34.4MCF) 632

Parachute (159 ft.) 240

Cutaway batt. box 5

Ladder 74

Truck plate 1

Rigging 10

SUNRISE Payload 21

Total: 983

SUNRISE Total Height at

Launch

Balloon diameter at float: 439 feet Flight train length at float: 726 feet

SCIENCE WEIGHT = 4232 lbs. CSBF ABOVE PIN = 964 lbs. CSBF BELOW PIN = 682 lbs. BALLAST = 1200 lbs. TOTAL ON BALLOON = 7078 lbs.


SUNRISE Test Flight 2009






Gondola Components

SUNRISE I


Gondola Components

SUNRISE I


Gondola Testing

SUNRISE I


Gondola Testing

SUNRISE I


Gondola Power System

SUNRISE I


Swedish Space Corporation, Kiruna, Sweden

SUNRISE I



SUNRISE I



SUNRISE I


Flight Path

SUNRISE I


Recovery

SUNRISE I


Recovery

SUNRISE I


Science Data

SUNRISE I

IMAX „Thumbnail“ image 4 x 4 binning (0.22 arcs/pix),

56 x 56 arcs2 FOV, 1.5 s integration time, Wavelength 525 nm,

RMS-contrast 12.6 %.

(Downloaded during flight)


Science Data

SUNRISE I


HIWIND

• The first FPI to measure daytime thermospheric winds. • Thermospheric winds are critical data for space weather research.


HIWIND


HIWIND


HIWIND


HIWIND


HIWIND


HIWIND G. Card, 2011 11 07


HIWIND


HIWIND


HIWIND


HIWIND


SUNRISE II


SUNRISE II


SUNRISE II


SUNRISE II


SUNRISE II

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Instrumentation from the Ground & Up Greg Card · Stratospheric Ballooning – SUNRISE & HIWIND...

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