The implications of runaway OB stars for high-mass star formation

Details The implications of runaway OB stars for high-mass star formation The implications of runaway OB stars for high-mass star formation

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.255..423c&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 255, April 1, 1992, p. 423-430.

Astronomy and Astrophysics

Astronomy

55

B Stars, Binary Stars, Mass Ratios, Massive Stars, O Stars, Star Formation, Star Distribution, Stellar Mass Ejection

Scientific paper

The properties of OB runaway stars assumed to be ejected from their parent clusters by dynamical binary-binary interactions are used to deduce certain necessary characteristics of high-mass star formation. It is deduced that massive stars form in small groups of binaries that are biased towards unit mass ratio, and that within these groups the IMF is severely under-represented in low-mass stars compared with the field star IMF.

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