Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.3203t&link_type=abstract
American Astronomical Society, DPS meeting #39, #32.03; Bulletin of the American Astronomical Society, Vol. 39, p.474
Astronomy and Astrophysics
Astronomy
Scientific paper
Stars form from the collapse of molecular clouds. The majority of gas in these clouds is not incorporated into stars, but remains intermixed with cluster for 5 Myr during star formation, before the gas and stars are dispersed. Young stars and disks orbiting through the cluster experience Bondi-Hoyle accretion from this reservoir, for a several Myr period after stars form but before the gas is dispersed. Accretion during the tail-end of star formation is at a much lower rate than the rapid collapse and competitive accretion of star formation itself. The late accretion from the cloud is predominantly onto the disk directly, because the disk intercepts the accretion flow before it can impact the star. We present simulations of Bondi-Hoyle accretion onto star-disk systems in three realistic model star clusters, with N=30, N=500, and N=3000 stars. We find mass accretion rates onto disks surrounding solar-mass stars are 2-5 10^-9 solar masses per year, or 1-3 MMSN disk masses in 5 Myr. The mass accreted is insignificant compared to the star's mass, but it is comparable to or greater than the disk mass. Although this mass, and its associated angular momentum, can have substantial impact on the evolution of young disks, it is not considered by standard models of the Solar nebula. We discuss a variety of implications of this process, including its effect on the formation of terrestrial and gas-giant planets, the migration of extrasolar planets, metallicity variations between a star and its planets, and the tilt of the Sun relative to the ecliptic plane. We also discuss observational implications.
Bally John
Throop Henry B.
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