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

Simon F.Portegies Zwart, Jasinta Dewi, Tom Maccarone

Research output: Contribution to journalArticlepeer-review

66 Scopus citations

Abstract

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.

Original languageEnglish
Pages (from-to)413-423
Number of pages11
JournalMonthly Notices of the Royal Astronomical Society
Volume355
Issue number2
DOIs
StatePublished - Dec 1 2004

Keywords

  • Binaries: close
  • Black hole physics
  • Galaxies: individual: M82
  • X-rays: binaries
  • X-rays: individual: M82 X-1

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