DPS 34th Meeting, October 2002
Session 10. Outer Planet Chemistry and Thermal Structure
Oral, Chair(s): G. Schubert and H. Hammel, Monday, October 7, 2002, 5:00-6:00pm, Room M

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[10.03] Inhomogeneous Evolution of Giant Planets: Jupiter and Saturn

J. J. Fortney, W. B. Hubbard (LPL -- U. of Arizona)

We present the first models of Jupiter and Saturn to couple their evolution to both a radiative-atmosphere grid and to high-pressure phase diagrams of hydrogen with helium and other admixtures. We find that prior calculated phase diagrams in which Saturnís interior reaches a region of predicted helium immiscibility do not allow enough energy release to prolong Saturnís cooling to its known age and effective temperature. We explore modifications to published phase diagrams that would lead to greater energy release, and propose a modified H-He phase diagram that is physically reasonable, leads to the correct extension of Saturnís cooling, and predicts an atmospheric helium mass fraction Yatmos = 0.185, in agreement with recent estimates. We also explore the possibility of internal separation of elements heavier than helium, and find that, alternatively, such separation could prolong Saturnís cooling to its known age and effective temperature under a realistic phase diagram and heavy element abundance (in which case Saturn's Yatmos would be solar but heavier elements would be depleted). In none of these scenarios does Jupiterís interior evolve to any region of helium or heavy-element immiscibility: Jupiter evolves homogeneously to the present day. We discuss the implications of our calculations for Saturn's primordial core mass.

This research was supported by Grants NAG5-10760 (NASA Astrophysics Theory Program), NAG5-10629 (NASA Origins of Solar Systems Program), and NAG5-8906 (NASA Planetary Geology and Geophysics Program).

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Bulletin of the American Astronomical Society, 34, #3< br> © 2002. The American Astronomical Soceity.