Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005ap%26ss.300..247p&link_type=abstract
Astrophysics and Space Science, Volume 300, Issue 1-3, pp. 247-253
Astronomy and Astrophysics
Astrophysics
4
Black Holes, Compact Objects, Simulation, Star Clusters, X-Ray Binaries
Scientific paper
The evolution of young (≲ 10 Myr) star clusters with a density exceeding about 105 star pc-3 are strongly affected by physical stellar collisions during their early lifetime. In such environments the same star may participate in several tens to hundreds of collisions ultimately leading to the collapse of the star to a black hole of intermediate mass. At later time, the black hole may acquire a companion star by tidal capture or by dynamical three-body capture. When the captured star evolves it starts to fill its Roche-lobe and transfers mass to its accompanying black hole. This then leads to a bright phase of X-ray emission, which lasts for the remaining main-sequence lifetime of the donor. If the star captured by the intermediate mass black hole is relatively low mass ≲ 2 M&sun;) the binary will also be visible as a bright source in gravitational waves. Based on empirical models we argue that, for as long as the donor remains on the main sequence, the source will be ultraluminous Lx >rsim 1040 ergs-1 for about a week every few month. When the donor star is more massive >15 M&sun;, or evolved off the main sequence the bright time is longer, but the total accretion phase lasts much shorter.
Dewi Jasinta
Maccarone Tom
Portegies Zwart Simon. F.
No associations
LandOfFree
Formation and Evolution of Intermediate Mass Black Hole X-Ray Binaries does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Formation and Evolution of Intermediate Mass Black Hole X-Ray Binaries, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Formation and Evolution of Intermediate Mass Black Hole X-Ray Binaries will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1835150