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Paper: Theoretical Developments in Understanding Massive Star Formation
Volume: 387, Massive Star Formation: Observations Confront Theory
Page: 189
Authors: Yorke, H.W.; Bodenheimer, P.
Abstract: 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 yr−1, stars of ∼5-10 M tend to bloat up to radii which may exceed 100 R. 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.
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