PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
For the next few weeks:
Terrestrial Planets, their Moons, and the Sun
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
Announcements
• Reading Assignment– Section 9-1 (pp 186-189) , 9-5 and 9-6 (pp 199-203)
• 3rd Homework is now posted on the course website (due Thursday 3/1)
• Term paper details are now posted on the website (due 4/17)
• Results from first exam will be briefly discussed today– Solutions will be posted soon
• Public Lecture next Tuesday (2/27) at 7:30PM in this auditorium– Prof. Bob Strom: “Global Warming”– There will be a sign-up sheet for students in this class. Sign in and
get 5pts extra-credit added to your in-class activities score for each one of these public lectures that you attend (including the first one, if you attended it)
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
First Exam Results
• Average: 69.1• Median: 70• High: 102-½ (5 scores over 99)• Total tests taken: 130
89 and above 18 (13.8%)
78 – 88 19 (14.6%)
67 – 77 38 (29.2%)
56 – 66 26 (20.0%)
55.5 and below 29 (22.3%)
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
First mid-term exam grade distribution
0
5
10
15
20
25
95-100 90-95 85-90 80-85 75-80 70-75 65-70 60-65 55-60 50-55 45-50 40-45 35-40 30-35 25-30
Series1
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
Approximate Curve
> 87.5 A (15.4%)
74 – 87 B (21.5%)
62.5 – 73.5 C (30.8%)
45 – 62 D (21.5%)
< 45 E (10.8%)
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
Today: Planetary Interiors and Surfaces
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
Review: Formation of terrestrial planets
• Small dust particles accreted to make “planetesimals”
• Planetesimals accreted (and collided with other planetesimals) to form protoplanets
• The protoplanets were at least partially molten– denser iron-rich material fell
to the center, bringing heavier metals with it, making an iron-rich core (differentiation)
– A terrestrial planet!
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
Internal structure of a terrestrial planet
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
All of the terrestrial planets, and Earth’s moon have a similar internal structure, but the relative sizes are different depending on how hot the interior got, how rapidly the object cooled, and how much mass it has
The largest factor in determining this structure is the object’s size
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
• Accretion– Conversion of gravitational energy of
incoming material to kinetic energy, into thermal energy
• Chemical Differentiation– Conversion of gravitational energy of
falling denser materials within the interior to thermal energy
• Radioactive decay of elements within the body’s interior– leads to a slight mass difference
between initial and final elements which is converted to energy E=Δmc2
Sources of heat
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
Cooling processes in terrestrial planets
• Mantle convection in the interior– Hot material rises, cold
material falls (like boiling water on a stove)
• Thermal conduction in the lithosphere– Like when a metal plate is
heated at one end – the other end will soon get hot too
• Radiative loss through the surface into space
• Volcanic eruptions
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
Probing the interiors of planets
• The only reliable way to accurately probe the interior of a planet is by analyzing seismic activity – like Earthquakes
• Another reasonable approach is to measure how the body rotates (by measuring its libration)
• The existence of a planetary magnetic field provides some basic information
• Theoretical and numerical models can be constructed, but these are not as definitive
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
Seismic Waves
• P and S waves (Primary and Secondary)– Move through the Earth’s
interior– Provide information
about interior’s structure
• Surface Waves– The rolling waves that
are felt on the surface– Like water waves
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
P- and S-waves
• P-waves– Compressional (or
longitudinal) waves– Can travel through
solids or liquids• S-waves
– Shear (or transverse) waves Cannot travel through liquids
P-waves, or compression waves
S-waves, or transverse waves
Water waves
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
• S-waves do not travel through the Earth’s core (creating a “shadow zone” as shown at below right)
• This proves that part of the core is liquid
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
• Another important tool for “probing” the interior of a planet
• Mercury – has a global magnetic field
– this is somewhat of a puzzle!
• Venus – does NOT have a global magnetic field
– Slow rotation rate
• Earth – has a very strong global magnetic field
• Mars – does not have a global magnetic field, but there is evidence that it had one in the past
Planetary Magnetic Fields
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
The Earth’s Dynamo
• Permanent magnets lose their field if raised to a temperature above about 500oC– The Earth is hotter than this
nearly everywhere
• Earth’s field is also known to change periodically– Pole reversals
• It must be generating its own internal magnetic field
• Need a circulating electric current – Circulation and convection of
electrically conductive molten iron in the Earth's outer core produces the magnetic field
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
Planetary Surfaces
• The appearance of a terrestrial planet’s surface is determined by internal geological activity, impacts with asteroids and comets, and erosion
• Examples of internal activity include:
– Plate tectonics and volcanism
• Atmospheres can give rise to both aeolian processes (wind erosion) and water erosion through precipitation and water flow, and other surface processes, such as the flow of glaciers
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
Evidence of Internal Activity: Volcanoes
• Volcanoes – either active or extinct – indicates whether the interior is currently active, or was so in the past
– Earth – active volcanoes – active interior
– Venus – possibly active volcanoes, (most are probably extinct) – active interior
– Mars – extinct volcanoes – no internal activity
– Mercury – no volcanoes – probably no internal activity
Olympus Mons, Mars
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
Evidence of Internal Activity: Plate Tectonics
• Plate tectonics is the shifting around of large crustal “plates” on the surface of a planet.– It is the result of convection in the
interior• Currently, only Earth has plate
tectonics
• One result of plate tectonics – huge mountain ranges
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
Aeolian processes
• Wind and water erosion have effected the surfaces of Earth, Mars, and Titan– Sand Dunes exist on all
three bodies– Dust devils exist on Mars
and Earth• Mars rover Sprit is still working
because of a dust devil! • Dust devils are much larger on
Mars
Dust devils on Mars
Sand dunes on Titan
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
Impact Cratering
• The dominant geological process in the solar system
• The number of craters on a body is a good indicator of the age of the surface
• Impacts have also affected the atmospheres of the gas giants
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
History of Craters
• Less than 100 years ago scientists felt that cratering due to impacts was unrealistic and highly improbable!– Volcanism was the
explanation (can see similar features associated with terrestrial volcanoes)
• 1960’s – consensus that impacts caused craters in solar-system bodies
“Crater” Elegante (Pinacate balsatic fields in Mexico, just below Arizona border)
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
Evidence for Craters due to
Impacts
• Shock effects in quartz (also seen in lunar rock samples) due to shock waves produced by the explosions associated with impacts
• Craters are nearly all circular in outline– raised rims, concentric inner terraces,
and other features that are seldom found in volcanic “craters”
– Circular also because of the shock waves associated with the explosion
• not elongated!
• Volcanic “craters” are usually very small and occur in a clearly volcanic environment.
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
Earth’s Impact Craters
• The Earth’s surface has probably received more impact events than the Moon– Earth is larger (but its
atmosphere burns up smaller ones).
• Only about 160 surviving craters
have been found thus far. So few because …– geological activity erases the
evidence (Earth’s surface is a young one)
– Earth’s atmosphere provides a shield against smaller asteroids Manicougan crater, Quebec, Canada
(5th largest crater in the world)
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
PTYS/ASTR 206 Planetary Surfaces and Interiors2/20/07
Earth’s Impact Craters