Volume 488, Number 3, September IV 2008
|Page(s)||1007 - 1015|
|Section||Stellar structure and evolution|
|Published online||17 July 2008|
Evolution of stellar collision products in open clusters
I. Blue stragglers in N-body models of M 67
Sterrekundig Instituut Utrecht, Postbus 80000, 3508 TA Utrecht, The Netherlands e-mail: email@example.com
2 Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn VIC 3122, Australia
Accepted: 4 June 2008
Stellar collisions are an important formation channel for blue straggler stars in globular and old open clusters. Hydrodynamical simulations have shown that the remnants of such collisions are out of thermal equilibrium, are not strongly mixed and can rotate very rapidly. Detailed evolution models of collision products are needed to interpret observed blue straggler populations and to use them to probe the dynamical history of a star cluster. We expand on previous studies by presenting an efficient procedure to import the results of detailed collision simulations into a fully implicit stellar evolution code. Our code is able to evolve stellar collision products in a fairly robust manner and allows for a systematic study of their evolution. Using our code we have constructed detailed models of the collisional blue stragglers produced in the N-body simulation of M 67 performed by Hurley et al. in 2005. We assume the collisions are head-on and thus ignore the effects of rotation in this paper. Our detailed models are more luminous than normal stars of the same mass and in the same stage of evolution, but cooler than homogeneously mixed versions of the collision products. The increased luminosity and inefficient mixing decrease the remaining main-sequence lifetimes of the collision products, which are much shorter than predicted by the simple prescription commonly used in N-body simulations.
Key words: stars: formation / stars: blue stragglers / Galaxy: open clusters and associations: general / methods: numerical / stars: evolution / stellar dynamics
© ESO, 2008
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