Physics
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufm.p54a..06h&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #P54A-06
Physics
5749 Origin And Evolution
Scientific paper
We model the effect of gradual dissipation of the protoplanetary disk on Jupiter's growth. The planet's structure is computed using a Henyey-type stellar evolution code. Previous simulations of this process have taken the radius of the planet to be approximately one Hill sphere radius, RH. Recent 3-D hydrodynamic simulations show that only gas within about 0.25 RH remains bound to the planet, with the more distant gas participating in the shear flow of the protoplanetary disk. Therefore, we computed Jupiter models for which the planet's radius is 0.25 RH. Results indicate that the smaller radius increases the time required for planetary growth by ~ 15%. Observations suggest that the typical lifetime of massive disks around young stellar objects is ~ 3 Myr. To account for the dissipation of such disks, we computed Jupiter models for which the surface gas density is decreased on this time scale and the maximum rate of gas flow onto the planet is taken from 3-D hydrodynamic simulations. Results of these simulations will also be presented.
Bodenheimer Peter
D'Angelo Gennaro
Hubickyj Olenka
Lissauer Jack . J.
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