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8 Atmospheric Evolution on Earth, Venus, and Mars

8 Atmospheric Evolution on Earth, Venus, and Mars

Tải bản đầy đủ - 39trang

6.8 Atmospheric Evolution on Earth, Venus, and Mars







Earth has a small greenhouse effect; it is

in equilibrium with a comfortable (for us)

surface temperature.



© 2017 Pearson Education, Inc.



6.8 Atmospheric Evolution on Earth, Venus, and Mars







Venus’s atmosphere is much denser and

thicker; a runaway greenhouse effect has

resulted in its present surface temperature

of 730 K.



© 2017 Pearson Education, Inc.



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, and 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.



© 2017 Pearson Education, Inc.



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 amounts of carbon dioxide in its atmosphere and closeness to the Sun led to a

runaway greenhouse effect and very hot surface.



© 2017 Pearson Education, Inc.



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 include the Tharsis bulge, Olympus Mons, Valles Marineris.

There is strong evidence for water on Mars in the past.



© 2017 Pearson Education, Inc.



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.



© 2017 Pearson Education, Inc.



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