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Chapter 6 The Terrestrial Planets

Chapter 6 The Terrestrial Planets. Units of Chapter 6. Orbital and Physical Properties Rotation Rates Atmospheres The Surface of Mercury The Surface of Venus The Surface of Mars Internal Structure and Geological History Atmospheric Evolution on Earth, Venus, and Mars Summary of Chapter 6.

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Chapter 6 The Terrestrial Planets

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  1. Chapter 6The Terrestrial Planets

  2. Units of Chapter 6 Orbital and Physical Properties Rotation Rates Atmospheres The Surface of Mercury The Surface of Venus The Surface of Mars Internal Structure and Geological History Atmospheric Evolution on Earth, Venus, and Mars Summary of Chapter 6

  3. 6.1 Orbital and Physical Properties The orbits of Venus and Mercury show that these planets never appear far from the Sun.

  4. The terrestrial planets have similar densities and roughly similar sizes, but their rotation periods, surface temperatures, and atmospheric pressures vary widely.

  5. 6.2 Rotation Rates Mercury can be difficult to image from Earth; rotation rates can be measured by radar.

  6. Mercury was long thought to be tidally locked to the Sun; measurements in 1965 showed this to be false. Rather, Mercury’s day and year are in a3:2 resonance; Mercury rotates three times while going around the Sun twice.

  7. Mars Venus

  8. All the planets rotate in a prograde direction, except Venus, which is retrograde.

  9. 6.3 Atmospheres Mercury has no detectable atmosphere; it is too hot, too small, and too close to the Sun. Venus has an extremely dense atmosphere. The outer clouds are similar in temperature to Earth, and it was once thought that Venus was a “jungle” planet. We now know that its surface is hotter than Mercury’s, hot enough to melt lead. The atmosphere of Mars is similar to Earth in composition, but very thin.

  10. 6.4 The Surface of Mercury Mercurycannot be imaged well from Earth; best pictures are from Messenger. Crateringon Mercury is similar to that on the Moon.

  11. Some distinctive features: Scarp(cliff), several hundred km long and up to 3 km high, thought to be formed as the planet cooled and shrank.

  12. Caloris Basin, very large impact feature; ringed by concentric mountain ranges

  13. 6.5 The Surface of Venus This map of the surface features of Venus is on the same scale as the Earth map below it.

  14. Venus as a globe, imaged by Magellan

  15. Top: Lava domes on Venus (L), and a computer reconstruction (R) Bottom: the volcano Gula Mons

  16. Venus corona, with lava domes

  17. A photograph of the surface, from the Veneralander

  18. Impact craters. Left: multiple-impact crater Above: Mead, Venus’s largest impact crater

  19. 6.6 The Surface of Mars Major feature: Tharsis bulge, size of North America and 10 km above surroundings Minimal cratering; youngest surface on Mars

  20. 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.

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

  22. Mars has largest volcano in Solar System; Olympus Mons: • 700 km diameter at base • 25 km high • Caldera 80 km in diameter Three other Martian volcanoes are only slightly smaller.

  23. Was there running water on Mars? Runoff channels resemble those on Earth. Left: Mars Right: Earth

  24. No evidence of connected river system; features probably due to flash floods

  25. This feature may be an ancient river delta. Or it may be something entirely different.

  26. Much of northern hemisphere may have been ocean.

  27. 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.

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

  29. 6.7 Internal Structure and Geological History Internal structure of Mercury, Mars, and the Moon, compared to Earth

  30. 6.8 Atmospheric Evolution on Earth, Venus, and Mars At formation, planets had primary atmosphere – hydrogen, helium, methane, ammonia, water vapor – which was quickly lost. Secondary atmosphere – water vapor, carbon dioxide, sulfur dioxide, nitrogen – comes from volcanic activity. Earth now has a tertiary atmosphere, 20 percent oxygen, due to the presence of life.

  31. Earth has a small greenhouse effect; it is in equilibrium with a comfortable (for us) surface temperature.

  32. Venus’s atmosphere is much denser and thicker; a runaway greenhouse effect has resulted in its present surface temperature of 730 K.

  33. the density of Mars is: A about like that of the Earth. B the lowest of the terrestrial planets. C the lowest of all planets. D the greatest of the terrestrial planets. 

  34. the rotational period of Venus was measured by A watching surface features move across the planet's disk B measuring the speed of clouds in the planet's atmosphere C measuring the Doppler shift of radar signals bounded off the planet's surf D orbiting spacecraft around the planet 

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

  36. the average surface temperature of Venus is: A about like that on Earth. B a bit warmer than that on Earth. C extremely hot because of a runaway greenhouse effect. D unknown since we have not explored the surface of Venus. 

  37. Venus' magnetic field produces which of the following A strong lightning discharges B strong auroral activity C a connection between the surface of Venus and that of its satellite D none of the above, since Venus has no significant magnetic field 

  38. comparing the interiors of the Earth and Mars, we can infer that A the Earth has a larger core of rocky materials. B Mars has a larger core of rocky materials. C the Earth has a larger core of metallic materials. D Mars has a larger core of metallic materials. 

  39. Summary of Chapter 6 • Mercury is tidally locked in a 3:2 ratio with the Sun. • Mercury has no atmosphere; Venus has a very dense atmosphere, whereas the atmosphere of Mars is similar to Earth in composition but very thin. • Mercury has no maria, but does have extensive intercrater plains and scarps.

  40. Summary of Chapter 6, cont. • Venus is never too far from the Sun, and is the brightest object in the sky (after the Sun and Moon). • It has many lava domes and shield volcanoes. • Venus is comparable to Earth in mass and radius. • Large amount of carbon dioxide in atmosphere, and closeness to the Sun, led to runaway greenhouse effect and very hot surface.

  41. Summary of Chapter 6, cont. • Northern and southern hemispheres of Mars are very different. • South is higher and heavily cratered. • North is lower and relatively flat. • Major features: Tharsis bulge, Olympus Mons, VallesMarineris • Strong evidence for water on Mars in the past

  42. Summary of Chapter 6, cont. • Mercury has very weak, remnant magnetic field. • Venus has none, probably because of very slow rotation. • Neither Venus nor Mars show signs of substantial tectonic activity.

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