Accretion Rates Of Planetesimals On A Jupiter-mass Planet

Details Accretion Rates Of Planetesimals On A Jupiter-mass Planet Accretion Rates Of Planetesimals On A Jupiter-mass Planet

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.2405d&link_type=abstract

American Astronomical Society, DPS meeting #42, #24.05; Bulletin of the American Astronomical Society, Vol. 42, p.958

Astronomy and Astrophysics

Astronomy

Scientific paper

We performed 3D calculations of the motion of a swarm of planetesimals in a protoplanetary disk that is perturbed by a Jupiter-mass planet. The interactions between the planet and the gaseous disk and the accretion of gas on the planet were modeled through a 3D hydrodynamics code. The trajectory of each planetesimal, in the gravitational field of the planet and of a solar-mass star, was determined by means of a 4th order Runge-Kutta algorithm that takes into account gas drag forces. Thermodynamics conditions that may apply to a protoplanetary disk towards the end of the planet's gas accretion epoch were used. The planetesimals were initially deployed on random Keplerian orbits about the star, between 1.1 and 1.5 planet's orbital radii. The gas dynamics around the planet was resolved on a length-scale of 0.01 planet's Hill radii (Rh). Planetesimals within a few tenths of Rh from the planet and whose velocity relative to the planet was smaller than the escape velocity were taken as accreted. Experiments were executed with a size distribution of an equal number of 1, 10, and 100 km radius planetesimals. The dynamics of the smallest size planetesimals appears to be more strongly affected by gas drag forces than it is that of planetesimals of larger sizes. However, results suggest that the accretion rates on the planet are of the same order of magnitude, once the initial surface density of planetesimals is corrected so that all size bins contain equal masses of solids. These rates, estimated at about 5 AU, are on the order of 1e-6 sigma Earth masses per year, where sigma is the solids' surface density of a given size bin, in grams per square centimeters, exterior of the planet's orbit. Support from NASA Origins of Solar Systems Program grants NNX08AH82G and NNX07AI72G is gratefully acknowledged.

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