Astronomy and Astrophysics – Astronomy
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21011303b&link_type=abstract
American Astronomical Society Meeting 210, #113.03; Bulletin of the American Astronomical Society, Vol. 39, p.238
Astronomy and Astrophysics
Astronomy
Scientific paper
We model 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 Hα light curves and the Hα emission profiles. The simulations have been carried out with a modified version of the parallel tree SPH code Gadget. The heating, cooling, and radiative processes have been calculated for two different physical scenarios, where the gas is approximated as a black-body or a solar metallicity gas. The calculation for the solar-metallicity scenario has been carried out with the photoionization code Cloudy. 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 the binary. The modeled Hα emission line profiles may be used as a criterion for selection of MBHB candidates from the existing archival data. The orbital period and mass ratio of a binary could be inferred from the Hα profiles of carefully monitored candidates. The discovery of sub-parsec binaries is an important step in understanding of the merger rates of MBHBs and their evolution towards the detectable gravitational wave window.
Bogdanovic Tamara
Eracleous Michael
Sigurdsson Steinn
Smith Daniel B.
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