Physics
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21822802g&link_type=abstract
American Astronomical Society, AAS Meeting #218, #228.02; Bulletin of the American Astronomical Society, Vol. 43, 2011
Physics
Scientific paper
We present the theoretical predictions for X-ray binary observations in young stellar environments, such as starbursts and young star clusters. Using a Monte Carlo method, we model realistic star clusters with ≈ 5 × 105 stars and significant binary fractions. Our code includes the physics of stellar and binary evolution, direct integration of close interactions, physical stellar collisions and tidal mass loss. Using this code we compute the formation rates and characteristic properties of single and binary BHs for various representative ages and choices of parameters. We find that, in general, more single BHs are formed and also retained in clusters, than BHs in binaries. We also find that the ejection of BHs from the cluster is a function of density, binary fraction and the number of stars in the cluster. For example, in low density clusters, it is mainly the initial supernovae kicks which eject BHs (low-mass stellar BHs) from the cluster, whereas in high density clusters more BHs (both low and high-mass stellar BHs) are ejected with dynamics. This leads us to speculate that the population of X-ray binaries in the vicinity of star clusters, is mainly from dense and massive clusters. We also use a stellar evolution code to calculate the luminosity of BH binaries ejected from the cluster and investigate the possibility of getting an observable X-ray binary from the cluster.
Goswami Sanghamitra
Rasio Frederic A.
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