Modeling the Radial Distribution of Blue Stragglers in M3

Details Modeling the Radial Distribution of Blue Stragglers in M3 Modeling the Radial Distribution of Blue Stragglers in M3

1994-06-01

arxiv.org/abs/astro-ph/9406004v1

Astronomy and Astrophysics

Astrophysics

14 pages, uuencoded postscript including 1 figure. Lick Observatory Preprint Series No. 27. To appear in the Astrophysical Jou

Scientific paper

10.1086/187486

Recent surveys of the blue straggler (BS) population in the galactic globular cluster M3 (NGC 5272) give the first complete characterization of the number density of BSs as a function of radius over an entire globular cluster. The BSs in M3 are overabundant at large radii, and significantly underabundant at intermediate radii. Here we present the result of a simulation of the dynamical evolution of a population of BSs in a multi--mass model of M3. Assuming the BSs were formed in the core through binary interactions (Hut \&\ Verbunt 1983, Leonard 1989, Sigurdsson \&\ Phinney 1993, Hut \etal 1992, Davies, Benz and Hills 1994), and given some very general assumptions about the recoil that occurs during stellar mergers in interacting binaries; we find an excellent fit to the observed radial distribution of BSs, suggesting strongly that most of the BSs in M3 were formed through binary collisions in the core.

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