Saturn1 - o only happens at cooler temperatures o may start...

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Saturn Introduction and General Properties   Saturn is a large planet mass = 95 x Earth volume = 380 x Earth albedo = 0.47 . . . . cloud covered density = 0.7 g/cm 3  . . . lowest of all planets => more like gas or liquid Motions orbit: orbital period = 29.5 years rotation: rotation period = 10.5 hours o very fast equator rotates faster than poles o "differential rotation" fast rotation flattens out the sphere at the poles - bulges at equator Interior observe strong magnetic field since it rotates quickly, expect liquid inside magnetic axis is aligned with rotation axis higly differentiated
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Figure 9.11 also show a cross section of Saturn.  [Link to Figure 9.11] source of heat inside planet emits 2 1/2 times the energy received from the Sun should have cooled faster than Jupiter o original heat should be gone heat from helium condensing to liquid and raining down inside planet
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Unformatted text preview: o only happens at cooler temperatures o may start to happen soon on Jupiter Atmosphere Composition: (from spectroscopy) hydrogen - 88 % helium - 11 % others - < 1 % similar to composition of original cloud that solar system formed from => very little change in atmosphere cloud region is more spread out on Saturn (from weaker gravity) Ciculation from: convection o mainly internal heat rather than Sun rotation see belts and zones as on Jupiter not as much color variation - so harder to see Figure 9.10 shows the belts and zones. [Figure 9.10] History basically the same as Jupiter ! Moons: 18 moons Figure 9.15 shows pictures of some of the moons discussed here. [Link to Figure 9.15] mainly ice all in synchronous orbit [except Hyperion (#16)]...
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This note was uploaded on 03/09/2012 for the course AST 1002 taught by Professor Emilyhoward during the Spring '10 term at Broward College.

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Saturn1 - o only happens at cooler temperatures o may start...

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