Comparisons between the accretion flows of low mass and high mass stars

Details Comparisons between the accretion flows of low mass and high mass stars Comparisons between the accretion flows of low mass and high mass stars

May 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...188.6404h&link_type=abstract

American Astronomical Society, 188th AAS Meeting, #64.04; Bulletin of the American Astronomical Society, Vol. 28, p.930

Physics

Scientific paper

There is a well-developed, observationally-tested paradigm for accretion flows around young stars, consisting of infall to a rotating circumstellar disk, followed by accretion through the disk onto the central star. Does this paradigm also apply to high-mass stars? Factors such as strong isotropic winds and radiation pressure could produce significant differences in the accretion physics of high- and low-mass stars. I shall outline the accretion paradigm for low mass stars, suggest how this might scale to the case of high mass star formation, and discuss some observational consequences of this scaling. I suggest that special environmental conditions are needed to form high-mass stars, and that these conditions may only be realized in regions where dense star clusters are formed.

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