Statistics – Computation
Scientific paper
Apr 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...389..546b&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 389, April 20, 1992, p. 546-557. Research supported by DOE and SNSF.
Statistics
Computation
63
Celestial Mechanics, Computational Astrophysics, Globular Clusters, Hydrodynamics, Main Sequence Stars, Three Dimensional Models, Binary Stars, Galactic Nuclei, Runge-Kutta Method, Stellar Mass
Scientific paper
A 3D smooth-particle hydrodynamic code with 7000 particles is used to simulate collisions between lower main sequence (MS) stars whose masses differ by a factor of five. Collisions between point-mass intruders and MS stars are simulated to study how the physics of the encounters depends on the finite radius of the smaller MS stars. It is found that the two MS stars become gravitationally bound in a physical collision if their relative velocity at infinity is less than a critical velocity Vd. Vd decreases from 1000 km/s in a head-on collision to 150 km/s in a grazing one. If the less massive star is replaced by a point mass, Vd remains the same for grazing collision and tidal encounters but drops to about 600 km/s in head-on collisions. The collision and coalescence of two MS stars resets the nuclear clock of the coalesced star, so it contracts to the MS. Tidal capture of binary stars in globular clusters can only occur in encounters in which the closest approach of the two stars to their center of mass is less than 2.0 times the sum of their radii.
Benz Willy
Hills Jack G.
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