Evolution of N-body systems with tidally captured binaries through the core collapse phase

Details Evolution of N-body systems with tidally captured binaries through the core collapse phase Evolution of N-body systems with tidally captured binaries through the core collapse phase

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...316..626s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 316, May 15, 1987, p. 626-659.

Statistics

Computation

63

Binary Stars, Globular Clusters, Stellar Motions, Computational Astrophysics, Ejection, Evolution (Development), Expansion, Gravitational Collapse

Scientific paper

A Fokker-Planck numerical code is used to compute the evolution of an idealized globular star cluster through the phases of collapse, bounce, and reexpansion. The cluster is initially composed of 3×105stars, each of mass 0.7 M_sun;, distributed as a Plummer model with core radius 0.8 pc. The model allows for the formation of close binaries via the two-body tidal-capture process and subsequent heating and ejection phenomena, but neglects the possibility of fusion into more massive stars. Collapse is reversed at t = 15 trh when the central density has increased by a factor of 103.5, due to the rapid ejection of binaries which have come to dominate the core. During reexpansion, the core regions may undergo overstable oscillations. Most of the ≡103 close tidally captured binaries present at core collapse are formed well before and ejected slowly afterward. During late stages, binary formation and ejection are nearly in equilibrium, with the cumulative ejection reaching one-fifth of the original mass by the end of the integration.

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