New Models for the Formation of Jupiter

Details New Models for the Formation of Jupiter New Models for the Formation of Jupiter

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000dps....32.6531h&link_type=abstract

American Astronomical Society, DPS Meeting #32, #65.31; Bulletin of the American Astronomical Society, Vol. 32, p.1645

Astronomy and Astrophysics

Astronomy

1

Scientific paper

New numerical simulations of the evolution and formation of Jupiter were computed. Earlier studies of the core instability model demonstrated that it was possible to form Jupiter with a solid core of 10 to 30 M⊕ within the lifetime of the protoplanetary disk (about 107 years). However, recent interior models of Jupiter suggest a core mass of about 5 M⊕ . We examine the effects of adjusting parameters to determine whether or not gas runaway can still occur for small mass cores. Halting planetesimal accretion at low core mass, which may simulate the presence of a competing embryo, will affect the gas accretion and the overall timescale. Decreasing the grain opacity to emulate the settling of grains within the protoplanetary atmosphere reduces the core mass required to form a giant planet within the lifetime of the protoplanetary disk. We computed three series of simulations. The first series included a baseline Jupiter model with an updated equation of state and opacity table and runs that stopped the planetesimal accretion onto the protoplanet with core masses of 10 M⊕ and 5 M⊕ . The second series of runs was computed with a grain opacity decreased by 1/50 of its nominal (solar composition) value. Here, too, extra runs were completed where the planetesimal accretion was stopped for cores of 10 M⊕ , 5 M⊕ , and 3 M⊕ . The final series of runs was computed with the reduced grain opacity and a reduced initial surface density of planetesimals in the solar nebula. For this last series there was only one run for which the solid accretion was cut off when the protoplanetary core reached 5 M⊕ . These models demonstrate the effects of opacity and core size on the evolution of giant planets. Reduction of the core mass size decreased the time for the protoplanet to evolve to its cross-over mass by as much as 50% in some cases as long as the core mass was not too small. Decreasing the grain opacity resulted in evolution times less than half of that for the baseline Jupiter model and evolutionary timescales increased when the solid surface density was decreased.

Affiliated with

Also associated with

No associations

Rating

New Models for the Formation of Jupiter does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with New Models for the Formation of Jupiter, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and New Models for the Formation of Jupiter will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1042085