Formation and Evolution of Giant Planet Accretion Disks

Details Formation and Evolution of Giant Planet Accretion Disks Formation and Evolution of Giant Planet Accretion Disks

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.0701w&link_type=abstract

American Astronomical Society, DPS meeting #38, #07.01; Bulletin of the American Astronomical Society, Vol. 38, p.491

Astronomy and Astrophysics

Astronomy

Scientific paper

The satellite systems of Jupiter and Saturn are thought to have formed from circumplanetary disks that surrounded these planets during their accretion. However, large satellites are susceptible to loss from rapid type I orbital decay due to strong disk torques. It has been proposed [1,2] that the current satellites are in fact the last survivors of continuing cycles of satellite formation and demise in an evolving viscous accretion disk, and that they accreted from material delivered from heliocentric orbit over a time interval of 10^5-10^6 years during the waning stage of giant planet formation. Here we place this so-called "starved disk” model within the context of giant planet formation models themselves, where the gas inflow rate decreases dramatically over the entire process. The discussion will be conducted using order-of-magnitude arguments, with the goal to evaluate the consistency of the starved disk model with early solar system events and its sensitivity to model characteristics such as disk viscosity, inflow rate, and planetary contraction histories.
This work is supported by the Outer Planets Research Program of NASA.
[1] Canup, R.M. & W.R. Ward Astron. J. 124, 3404 (2002); [2] Canup, R.M. & W.R. Ward Nature 441 834 (2006).

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