TY - JOUR
T1 - Intermediate mass black holes in accreting binaries
T2 - Formation, evolution and observational appearance
AU - Zwart, Simon F.Portegies
AU - Dewi, Jasinta
AU - Maccarone, Tom
PY - 2004/12/1
Y1 - 2004/12/1
N2 - 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 (∼1 keV) blackbody temperature. We perform detailed binary evolution calculations of 2-15 M⊙ stars which transfer mass to a 100-2000 M⊙ 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-l is a 10-15 M ⊙ star near the end of its main sequence or slightly evolved, which transfers mass to a ∼1000 M⊙ 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.
AB - 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 (∼1 keV) blackbody temperature. We perform detailed binary evolution calculations of 2-15 M⊙ stars which transfer mass to a 100-2000 M⊙ 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-l is a 10-15 M ⊙ star near the end of its main sequence or slightly evolved, which transfers mass to a ∼1000 M⊙ 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.
KW - Binaries: close
KW - Black hole physics
KW - Galaxies: individual: M82
KW - X-rays: binaries
KW - X-rays: individual: M82 X-1
UR - http://www.scopus.com/inward/record.url?scp=10444221013&partnerID=8YFLogxK
U2 - 10.1111/j.1365-2966.2004.08327.x
DO - 10.1111/j.1365-2966.2004.08327.x
M3 - Article
AN - SCOPUS:10444221013
SN - 0035-8711
VL - 355
SP - 413
EP - 423
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 2
ER -