Collisions and close encounters between massive main-sequence stars

Details Collisions and close encounters between massive main-sequence stars Collisions and close encounters between massive main-sequence stars

Aug 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...412..593l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 412, no. 2, p. 593-611.

Astronomy and Astrophysics

Astrophysics

33

Globular Clusters, Main Sequence Stars, Massive Stars, Stellar Mass Ejection, Stellar Motions, Density Distribution, Galactic Nuclei, Stellar Interiors

Scientific paper

Smooth-particle hydrodynamics is used to investigate collisions and close encounters between two massive main-sequence stars. Approximate scaling relations and fitting formulas are given for the amount of mass loss and for the critical impact parameters for capture or merging. The more massive stars, which have smaller ratios of specific binding energy to the square of escape velocity, are more easily disrupted in collisions. As the relative velocity increases, the orbital energy of the colliding stars can only be dissipated by shock heating, and the critical capture radius decreases much faster than predicted by linear theory. The average fractional mass loss per collision in a cluster is found not to depend sensitively on the stellar velocity dispersion.

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