Phase Separation in Giant Planets: Inhomogeneous Evolution of Saturn

Details Phase Separation in Giant Planets: Inhomogeneous Evolution of Saturn Phase Separation in Giant Planets: Inhomogeneous Evolution of Saturn

2003-05-01

arxiv.org/abs/astro-ph/0305031v1

Icarus 164 (2003) 228-243

Astronomy and Astrophysics

Astrophysics

33 pages, Accepted to Icarus

Scientific paper

10.1016/S0019-1035(03)00130-1

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 Saturn's interior reaches a region of predicted helium immiscibility do not allow enough energy release to prolong Saturn's 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 Saturn's cooling, and predicts an atmospheric helium mass fraction Y_atmos = 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 Saturn's cooling to its known age and effective temperature under a realistic phase diagram and heavy element abundance (in which case Saturn's Y_atmos would be solar but heavier elements would be depleted). In none of these scenarios does Jupiter's 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.

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