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Core dissolution and the dynamics of massive stars in young stellar clusters

Published online by Cambridge University Press:  22 December 2003

C. Boily ,
P. Patsis ,
S. Portegies ,
R. Spurzem ,
C. Theis ,
S.G. Vine  and
I.A. Bonnell
S.G. Vine
Affiliation:
School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KY16 9SS
I.A. Bonnell
Affiliation:
School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KY16 9SS
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Abstract

Massive stars are found, and, because of their age, are probably formed,in cluster cores. When the stars begin to shine, strong stellarwinds of ≳ 103 km s-1 exert a tremendous force on any remaining gas,which has at the same time been heated and expands at the sound speed(~10 km s-1). The gas will be rapidly expelled fromcluster core in much less than a core crossing time. This reduces thepotential of the core, dramatically affecting the dynamics of the corestars. This process is simulated using NBODY2 to follow thedistributions of massive stars over a few crossing times for variousinitial gas fractions. The core of massive stars is found to remainintact for a core gas fraction of 4 (or equivalently, a star formationeffeciency of 20%). The space and velocity distributions are alsoinvestigated.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 10: JENAM 2002, Galactic & Stellar Dynamics , 2003 , pp. 175
Copyright
© EAS, EDP Sciences, 2003

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