Intermediate mass black holes in accreting binaries: formation, evolution and observational appearance

被引:80
作者
Portegies Zwart, S
Dewi, J
Maccarone, T
机构
[1] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands
[2] Univ Amsterdam, Sect Computat Sci, NL-1012 WX Amsterdam, Netherlands
[3] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England
关键词
black hole physics; binaries : close; galaxies : individual : M82; X-rays : binaries; X-rays : individual : M82 X-1;
D O I
10.1111/j.1365-2966.2004.08327.x
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We study the origin of the ultraluminous X-ray source M82 X-1 in the nearby starburst galaxy M82. This X-ray source is of particular interest as it is currently the best candidate for an intermediate mass black hole; it is associated with a 54 mHz quasi-periodic oscillation with a relatively low (similar to1 keV) blackbody temperature. We perform detailed binary evolution calculations of 2-15 M-circle dot stars which transfer mass to a 100-2000 M-circle dot black hole and present an empirical model for the X-ray characteristics expected for such binaries. Based on the binary evolution calculations and the assumption in our simulations we conclude that the most likely candidate for the bright X-ray source M82 X-1 is a 10-15 M-circle dot star near the end of its main sequence or slightly evolved, which transfers mass to a similar to1000 M-circle dot black hole. We expect the system to be in the high/soft state. In that case the binary will not be visible as a source of gravitational wave radiation, but other transient X-ray binaries with lower mass donors way be rather bright sources of gravitational wave radiation.
引用
收藏
页码:413 / 423
页数:11
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