HR: 17:15h
AN: P54A-06    [Abstracts]
TI: Formation of Jupiter via Core Nucleated Accretion Within a Dissipating Protoplanetary Disk
AU: * Hubickyj, O
EM: hubickyj@pollack.arc.nasa.gov
AF: UCO/Lick Observatory -- NASA Ames Research Center, 1156 High St., Santa Cruz, CA 95064, United States
AU: Lissauer, J J
EM: jlissauer@mail.arc.nasa.gov
AF: NASA Ames Research Center, M.S. 304, Moffett Field, CA 94035, United States
AU: D'Angelo, G
EM: gdangelo@arc.nasa.gov
AF: NASA Ames Research Center, M.S. 304, Moffett Field, CA 94035, United States
AU: Bodenheimer, P
EM: peter@ucolick.org
AF: UCO/Lick Observatory -- NASA Ames Research Center, 1156 High St., Santa Cruz, CA 95064, United States
AB: 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, R_H. Recent 3-D hydrodynamic simulations show that only gas within about 0.25 R_H 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 R_H. 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.
DE: 5749 Origin and evolution
SC: Planetary Sciences [P]
MN: 2007 Fall Meeting