Observational Signatures of Massive Black Hole Binaries

Details Observational Signatures of Massive Black Hole Binaries Observational Signatures of Massive Black Hole Binaries

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.0781s&link_type=abstract

American Astronomical Society, HEAD meeting #9, #7.81; Bulletin of the American Astronomical Society, Vol. 38, p.1292

Astronomy and Astrophysics

Astronomy

Scientific paper

We modeled the electromagnetic signatures of massive black hole binaries (MBHBs) with an associated gas component. The method comprises numerical simulations of relativistic binaries and gas coupled with calculations of the physical properties of the emitting gas. We calculate the UV/X-ray and the HIα light curves and the HIα emission line profiles. The simulations have been carried out with a modified version of the parallel tree SPH code Gadget (Springel 2005). The heating, cooling, and radiative processes have been calculated for three different physical scenarios, where the gas is approximated as a black-body, a hydrogen-helium gas, or a solar metallicity gas. The calculation for the solar metallicity scenario has been carried out with the photoionization code Cloudy (Ferland et al. 1998). We investigate the sub-parsec binaries which have not yet entered the gravitational radiation phase. The results from the first set of calculations, carried out for a coplanar binary and gas disk, suggest that the outbursts in the X-ray light curve are pronounced during pericentric passages and can serve as a fingerprint for this type of binaries if periodic outbursts are a long lived signature of a binary. The modeled HIα emission line profiles may be used as a criterion for selection of MBHB candidates from the existing archival data

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