Key points: Terrestrial and giant planets; range of properties with distance from sun and what drives them; retention of gas and atmospheres
The Planets to Scale; from the sun, the "terrestrial planets" are Mercury, Venus, Earth, and Mars, while the "giant planets" are Jupiter, Saturn, Uranus, and Neptune (Pluto was an oddity at the end*). (from http://www.adamnieman.co.uk/futurelab/)
*On August 24, 2006, the International Astronomical Union - the body that oversees such matters - voted to strip Pluto of its planet status. By official decree, we now have only eight planets.
Here is a rough comparison of their interior structures. They are all variations on a common theme, with solid iron cores inside liquid iron components (except for Mars, where the interior temperature is too low to liquify this zone), surrounded by mantles of silicate rock, overlaid with rocky crusts.
Distances from the sun range from about 5 AU (Jupiter) to 30 AU (Neptune)
Average densities are low, similar to water: Jupiter is 1.3 grams/cm3 and Saturn is 0.7 grams/cm3
Composition similar to Sun -- (especially Jupiter and Saturn)
Liquid or icy surfaces
Dense atmospheres with violent and long lasting storms
Strong magnetic fields (Jupiter and Saturn)
|Here is a comparison of their interiors
They are all built around rocky cores. The interiors of
Jupiter and Saturn feature liquid metallic hydrogen (possible because of the
immense interior pressures) and then non-metallic liquid hydrogen. The
distinction is that the metallic form is electrically conducting.
Uranus and Neptune are largely icy. All these planets have gaseous hydrogen
atmospheres at the top.
The Earth is shown for comparison. It is not very different in mass from the rocky/metallic cores of the giant planets, indicating that all the planets started with similar reservoirs of raw material. The differing properties have to arise from how the planets formed from these reservoirs.
|The densities and compositions of the planets are correlated with how close they are to the sun, and hence the temperature at which they had to form. (From The Essential Cosmic Perspective, by Bennett et al.)|
Low density ices could only condense in the zone of giant planets, where temperatures were low. (by G. Rieke, some data from Univ. of Michigan Global Change Program, http://www.sprl.umich.edu/GCL/)
The average speed of an atom or molecule goes as the square root of the temperature divided by the mass of the particle. If the speeds are close to the escape velocity, gases will leak away into space. At the high temperatures at the orbit of Mercury (and its relatively small gravity), all gaseous materials escaped. For Venus and Earth, the lower temperature and larger gravity allowed heavier gases to be retained (oxygen, nitrogen) but hydrogen and helium escaped. Mars lost most of its gases because its surface gravity is small. The giant planets were out where temperatures were low enough to retain virtually all the gases.
The ice line for the Solar System lies between Mars and Jupiter. It marks a major divide in planet properties because outside of it, various kinds of frozen light molecules could accumulate on a forming planet as ices (for example, frozen water captures not only oxygen, but some hydrogen). These ices ran up the mass of the planet so it had a chance to retain the light gases, even helium and hydrogen. Thus, the giant planets (around the sun AND the other stars) probably all had to form outside of the frost line.
How do planetary systems form
Test your understanding before going on
|Formation of the sun and moon, ceiling painting, St. Isaac's Cathedral, St. Petersburg (photo by G. Rieke)||
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hypertext G. H. Rieke
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