1. Chapter 6 Exploring Terrestrial Surface Processes and Atmospheres

2. Terrestrial Planet Surfaces, the Same Yet Different
Craters
Heavily cratered areas and smooth low-lying plains
A few thousand, evenly distributed
A few hundred
Volcanoes
None
Many at hot spots, some possibly active
Many active, primarily at plate boundaries
Many at hot spots, all inactive
Atmosphere
Very thick
Just right!
Very thin

3. Impact Craters
An impactor colliding with the Moon generates a shock wave in the lunar surface that spreads out from the point of impact.
Produces a nearly perfectly circular crater, no matter in what direction the incoming impactor moves.
Many of the larger lunar craters also have a central peak, characteristic of a high-speed impact.

4. Cratering Measures Geologic Activity
Not all planets and satellites show the same amount of cratering.
Geological activity erases cratering:
Plate tectonic
Weathering
Erosion

5. Geologic activity seems to vary with size.
Larger bodies cooled more slowly, allowing craters to be erased

6. Geology of Mercury
The Caloris Basin, a crater 1300 km (810-mi) in diameter
The impact fractured the surface extensively, forming several concentric chains of mountains. The mountains in the outermost ring are up to 2 km (6500 ft) high

7. Cratering recorded gravitational shifts in the solar system.
Cratering dropped as the solar system “cleared up” then spiked again.
Jupiter/Saturn shifting in their orbit?

8. Heavy Hits During the Late Heavy Bombardment
Some impacts were so intense they weakened the Moon’s crust, leading to cracks where lava welled up and filled the crater.

9. Tectonics on Venus: A Thin Crusty

10. A Topographic Map of Venus
Radar altimeter measurements by Magellan were used to produce this topographic map of Venus. Flat plains of volcanic origin cover most of the planet’s surface, with only a few continent like highlands.
Why can’t we just take pictures?

11. Tectonics on Mars: A Thick, Rigid Crust
Mars: no global network of ridges and subduction zones
The entire crust of Mars makes up a single tectonic plate?
Magma moving beneath the crust? Magma plumes?

12. Hot Spots on Mars
Olympus Mons is the largest volcano in the solar system.
The base of Olympus Mons measures 600 km (370 mi) in diameter, and the scarps (cliffs) that surround the base are 6 km (4 mi) high.
The caldera, or volcanic crater, at the summit is approximately 70 km across, large enough to contain the state of Rhode Island.

13. Valles Marineris
The huge rift valley of Valles Marineris, 4000 km (2500 mi) long and 600 km (400 mi) wide at its center. Its deepest part is 8 km (5 mi).
This perspective image from the Mars Express spacecraft shows what you would see from a point high above the central part of Valles Marineris.

14. A Topographic Map of Mars
Most of the southern hemisphere is higher than the northern hemisphere.
The landing sites for probes on Mars are marked with an X.

15. Volcanoes on Venus, Earth, and Mars

16. Plate Tectonics on the Terrestrial Planets
Volcanoes
None
Many at hot spots, some possibly active
Many active, primarily at plate boundaries
Many at hot spots, all inactive
Crust
Very Very Thick
SOLID!
Very Thin
Just right!
Very Thick
Plate Tectonics No
Yes

17. Atmospheres surrounding terrestrial planets vary considerably.
These atmospheres all began with materials outgassed by volcanoes.
How did they become so different?

18. Venus: A Broiled Planet
Bathed in more intense sunlight than Earth because it is closer to the Sun.
Too hot to rain liquid water: water is trapped as clouds.
Water vapor is a greenhouse gas, trapping heat from the Sun.

19. The Martian Atmosphere: Not a Drop to Drink
CO2 levels dropped, cooling the planet:
runaway icehouse effect

20. Water may have once existed on the surface of Mars.
A network of dry riverbeds extending across the cratered southern highlands.
Teardrop-shaped islands rise above the floor of Ares Valles, carved out by a torrent of water that flowed from the bottom of the image toward the top.

21. Looking for Water on Our Moon
SDI-NASA Clementine spacecraft found some evidence of possible ice at the Moon’s poles.
Lunar Prospector found similar, but still inconclusive, evidence for water.
LCROSS purposefully crashed into the Moon’s pole and caused an explosive plume of debris to be ejected high above the surface.
Water was observed among the ejected debris.

22. Europa: What lies beneath its icy crust?
Infrared spectrum shows a thin layer of fine-grained water ice frost on top of a surface of pure water ice.
Jupiter gravitational influence cause “squeezing,” keeping the ocean warm.

23. Other Signs of an Underground Ocean