Intermediate mass black holes in accreting binaries: formation, evolution and observational appearance
| Autor: | Thomas J. Maccarone, Jasinta D. M. Dewi, Simon Portegies Zwart |
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| Přispěvatelé: | High Energy Astrophys. & Astropart. Phys (API, FNWI), Computational Science Lab (IVI, FNWI) |
| Rok vydání: | 2004 |
| Předmět: |
Physics
Gravitational wave Astrophysics::High Energy Astrophysical Phenomena Astrophysics (astro-ph) FOS: Physical sciences Binary number Astronomy and Astrophysics Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Radiation Galaxy Black hole General Relativity and Quantum Cosmology Stars Space and Planetary Science Intermediate-mass black hole Quasi periodic Astrophysics::Galaxy Astrophysics |
| Zdroj: | Monthly Notices of the Royal Astronomical Society, 355, 413-423. Oxford University Press |
| ISSN: | 0035-8711 |
| Popis: | We study the origin of the ultraluminous X-ray source M82-X1 in the nearby starburst galaxy M82. This X-ray source is of particular interest as it is currently the best candidate intermediate mass black hole; it is associated with a 54mHz quasi periodic oscillations with a relatively low (~1keV) black-body temperature. We perform detailed binary evolution calculations of 2--15Msun stars which transfer mass to a 100--2000Msun 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-X1 is a 10-15Msun star near the end of its main-sequence or slightly evolved, which transfers mass to a ~1000Msun 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. Comment: in press: 2004, MNRAS volume 481 (erratum added) |
| Databáze: | OpenAIRE |
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