Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.6002b&link_type=abstract
American Astronomical Society, DPS meeting #39, #60.02; Bulletin of the American Astronomical Society, Vol. 39, p.536
Astronomy and Astrophysics
Astronomy
Scientific paper
The core accretion mechanism for gas giant planet formation requires multiple-Earth-mass protoplanets to form in the presence of the disk gas, i.e., prior to the dispersal of the protoplanetary disk. Such protoplanets are subject to rapid orbital migration through their gravitational interactions with the disk. Studies of the interactions of Earth-mass protoplanets with the disk gas generally assume a disk mass low enough that the disk's self-gravity can be neglected. However, forming Earth-mass cores prior to the dissipation of the gaseous disk may require a disk that is massive enough ( 0.1 solar mass) to be marginally gravitationally unstable. In this case, the self-gravity of the disk must be taken into account when attempting to follow the orbital evolution of the growing protoplanets. We present here the results of a new set of three dimensional gravitational radiation hydrodynamics models of protoplanetary disks in which Earth-mass protoplanets are assumed to have formed by collisional accumulation, the first step of the core accretion mechanism. The models allow the protoplanets to gravitationally interact with the disk and to undergo orbital evolution as a result. The self-gravitating disk's evolution is influenced by the gravity of the protoplanets as well. Models have been calculated where the mass of the protoplanet is 0.01, 0.1, 1.0, or 10.0 Earth masses, for a disk with a mass of 0.09 solar masses orbiting a solar-mass protostar. The protoplanets start on circular orbits with semi-major axes of 6, 8, 10, and 12 AU. Because the protoplanet masses are small compared to the disk mass, all four masses evolve in a similar manner, with eccentricities growing to 0.1 to 0.3. No monotonic trends are evident during the first several hundred years, suggesting that such planets may be orbitally stable during this phase.
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