Astronomy and Astrophysics – Astronomy
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aspc..387..189y&link_type=abstract
Massive Star Formation: Observations Confront Theory ASP Conference Series, Vol. 387, proceedings of the conference held 10-14 S
Astronomy and Astrophysics
Astronomy
15
Scientific paper
Except under special circumstances massive stars in galactic disks will form through accretion. The gravitational collapse of a molecular cloud core will initially produce one or more low-mass quasi-hydrostatic objects of a few Jupiter masses. Through subsequent accretion the masses of these cores grow as they simultaneously evolve toward hydrogen-burning central densities and temperatures. We review the evolution of accreting (proto-)stars, including new results calculated with a publicly available stellar evolution code written by the authors. The evolution of accreting stars depends strongly on the accretion history. We find that for the high accretion rates considered, ˜10^{-3} M_&sun;yr^{-1}, stars of ˜5-10 M_&sun; tend to bloat up to radii which may exceed 100 R_&sun;. Because of the high rate of binarity among massive stars, we expect that these large radii during short phases of evolution will result in mass transfer, common envelope evolution, and a higher number of tight binaries with periods of a few days.
Bodenheimer Peter
Yorke Harold W.
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