Chapter 10: Mars

1. Chapter 10: Mars

2. Units of Chapter 10 10.1 Orbital Properties 10.2 Physical Properties 10.3 Long-Distance Observations of Mars 10.4 The Martian Surface 10.5 Water on Mars Life on Mars? 10.6 The Martian Atmosphere 10.7 Martian Internal Structure 10.8 The Moons of Mars

3. 10.1 Orbital Properties Mars’s orbit is fairly eccentric which affects amount of sunlight reaching it When viewed from Earth, Mars can be located either in the general direction of the Sun (conjunction) or away from it (opposition).

4. 10.2 Physical Properties Radius: 3394 km Moons: Deimos, Phobos Mass: 6.4 x 1023 kg Density: 3900 kg/m3 Length of day: 24.6 hours

5. 10.3 Long-Distance Observationsof Mars From Earth, can see polar ice caps that grow and shrink with the seasons Much better pictures from Mars missions, close-up

6. Changing polar ice caps are frozen carbon dioxide; water ice is permanently frozen • Shifting dust cover makes surface look like it is changing • Frequent dust storms, with high winds

7. 10.4 The Martian Surface Major feature: Tharsis bulge, size of North America and 10 km above surroundings Minimal cratering; youngest surface on Mars

8. This map shows the main surface features of Mars. There is no evidence for plate tectonics.

9. Northern hemisphere (left) is rolling volcanic terrain • Southern hemisphere (right) is heavily cratered highlands; average altitude 5 km above northern • Assumption is that northern surface is younger than southern • Means that northern hemisphere must have been lowered in elevation and then flooded with lava

10. VallesMarineris: Huge canyon, created by crustal forces Top right: Grand Canyon on same scale • 4000 km long • Maximum 120 km wide, 7 km deep

11. Mars has largest volcano in solar system: Olympus Mons • 700 km diameter at base • 25 km high • Caldera is 80 km in diameter Three other Martian volcanoes are only slightly smaller

12. 10.5 Water on Mars Was there running water on Mars? Runoff channels resemble those on Earth Left: Mars Right: Louisiana

13. Current thinking: Open water (rivers, lakes) once existed on Mars

14. This may be an ancient Martian river delta (or it may not)

15. Much of northern hemisphere may have been ocean

16. Impact craters less than 5 km across have mostly been eroded away Analysis of craters allows estimation of age of surface Crater on right was made when surface was liquid

17. Recently, gullies have been seen that seem to indicate the presence of liquid water; interpretation is still in doubt

18. More intriguing, this pair of images appears to show that gully formation is ongoing

19. Some water may now be permafrost under polar ice caps Left: Southern polar cap, mostly carbon dioxide Right: Northern polar cap, mostly water Both images taken during local summer

20. Viking landers both landed in low-latitude northern plains Rocky surface, red due to iron content Viking 1

21. Viking 2

22. The landing site for Opportunity was chosen to maximize the chances of finding water, or evidence for water

23. Discovery 10-1: Life on Mars? Viking landers looked for evidence of living organisms; did not find anything conclusive

24. Discovery 10-1: Life on Mars? Two Martian meteorites found in Antarctica show possible signs of microbial life, but evidence is disputed Three-part figure frm right page of Discovery 10-1 goes here

25. 10.6 The Martian Atmosphere Martian atmosphere is mostly carbon dioxide, and very thin Too thin to retain much heat; temperature drops sharply at night

27. Fog can form in low-lying areas, as sunlight strikes

28. Mars may be victim of runaway greenhouse effect in the opposite sense of Venus’s. As water ice froze, Mars became more and more reflective and its atmosphere thinner and thinner, freezing more and more water and eventually carbon dioxide as well.

29. As a result, Mars may have had a thicker atmosphere and liquid water in the past, but they are now gone.

30. 10.7 Martian Internal Structure • No seismic studies have been done • From behavior of crust, it is estimated to be 100 km thick • No magnetic field, so core is probably not metallic, not liquid, or neither liquid nor metallic

31. 10.8 The Moons of Mars Mars has two tiny moons: Phobos (left, 28 km x 20 km) Deimos (right, 16 km x 10 km) Both probably captured from the asteroid belt

32. The oldest regions on the Martian surface are those with • polar caps. • volcanoes. • impact craters. • arroyos. 

33. The Earth has a strong planetary magnetic field, in contrast to Mars, which has a very weak field, if any at all. in the context of the dynamo model, we can explain this difference by noting that Mars rotates very slowly. Mars is farther from the sun than the Earth. the interior of Mars is very hot. the interior of Mars is mostly rocky materials. 

34. The density of Mars is: about like that of the Earth. the lowest of the terrestrial planets. the lowest of all planets. the greatest of the terrestrial planets. 

35. Amajor feature of the atmosphere of Mars is very dense clouds shrouding most of the planet. strong winds and dust storms. very high temperatures and pressures. chemical mixture very similar to that of Earth.

36. Which of the following did not, directly or indirectly, result from large-scale volcanic eruptions on Mars in the past? Large shield volcanoes. Water vapor in the atmosphere. Polar icecaps. Impact craters, mostly in the southern hemisphere. Carbon dioxide in the atmosphere. 

37. Mars is orange because dust in the atmosphere reflects orange light the most effectively. the surface is littered with orange peels from an ancient (and stupid) civilization. the soil is radioactive and therefore glows orange. the soil is rusty because of the presence of ferrous oxide.

38. Olympus Mons is the widest canal discovered on Mars. a Martian sea, although it no longer has water in it. a Martian volcano, twice the height of Mt. Everest. the largest impact crater on Mars.

39. We would expect Mars to undergo seasonal changes much like those on Earth because Mars is about the same distance from the sun as Earth. Mars' equator is inclined to its orbital plane about the same as Earth's. the same calendar is used on Mars as on Earth. Mars rotates about as fast as the Earth does.

40. In general, impact craters on the surface of Mars are shallower than those on our moon, and its moons Deimos, and Phobos . This fact implies that smaller objects hit the surface of Mars. the Martian surface is harder than the others. more erosion has occurred on Mars than the moons. Mars quakes have made the crater walls collapse. objects hit Mars with a lower velocity. 

41. Summary of Chapter 10 • Mars’s orbit is more eccentric than Earth’s • Rotates in 24.6 hours; axial tilt similar to Earth’s • Atmosphere very thin, mostly carbon dioxide • Temperature averages 50 K below Earth’s, but seasons are otherwise similar • Mars landers have yielded substantial amounts of data

42. Summary of Chapter 10 (cont.) • Northern and southern hemispheres are very different • South is higher and heavily cratered • North is lower and relatively flat • Major features: Tharsis bulge, Olympus Mons, VallesMarineris • Crater ejecta provide evidence for permafrost layer under surface (easily liquidized) • Two small moons, probably captured asteroids