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Theoretical developments in understanding massive star formation

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dc.contributor.author Yorke, Harold W.
dc.contributor.author Bodenheimer, Peter
dc.date.accessioned 2011-02-08T21:25:21Z
dc.date.available 2011-02-08T21:25:21Z
dc.date.issued 2007-09-10
dc.identifier.citation Massive star formation: observations confront theory, September 10, 2007, Heidelberg, Germany en_US
dc.identifier.clearanceno 08-0177
dc.identifier.uri http://hdl.handle.net/2014/41704
dc.description.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. en_US
dc.description.sponsorship Max-Planck-Society en_US
dc.publisher Pasadena, CA : Jet Propulsion Laboratory, National Aeronautics and Space Administration, 2008. en_US
dc.subject star formation en_US
dc.subject stellar evolution en_US
dc.subject accretion en_US
dc.title Theoretical developments in understanding massive star formation en_US
dc.type Preprint en_US


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