Formation and Evolution of Intermediate Mass Black Hole X-Ray Binaries |
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Authors: | Simon F Portegies Zwart Jasinta Dewi Tom Maccarone |
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Institution: | (1) Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, Kruislaan 403, Amsterdam, The Netherlands;(2) Institute for Computer Science, University of Amsterdam, Kruislaan 403, Amsterdam, The Netherlands;(3) Department of Astrophysics, University of Oxford, Keble Road, Oxford, OX1 3RH, UK |
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Abstract: | 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⊙) 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⊙, or evolved off the main sequence the bright time is longer, but the total accretion phase lasts much shorter. |
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Keywords: | black holes compact objects simulation star clusters X-ray binaries |
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