Magnetized Accretion onto Inspiraling Binary Black Holes: II. Disk Dynamics

Details Magnetized Accretion onto Inspiraling Binary Black Holes: II. Disk Dynamics Magnetized Accretion onto Inspiraling Binary Black Holes: II. Disk Dynamics

Mar 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aps..apr.g8003n&link_type=abstract

American Physical Society, APS April Meeting 2012, March 31-Apr 3, 2012, abstract #G8.003

Physics

Scientific paper

The coincident observation of electromagnetic and gravitational wave signals from supermassive black hole (BH) mergers would provide a bounty to physics: e.g., a new redshift-distance measurement, improved source localization, and tighter constraints on source parameters (e.g., BH masses, BH spins, disk characteristics). Previous simulation work has focused on the two extremes: very close to merger where numerical relativity is required, or at large binary separations where Newtonian gravity theory is accurate. Our work here investigates an intermediate regime, where the post-Newtonian (PN) approximation is valid yet close enough so that separation shrinkage timescale is comparable to matter inflow timescales. With our PN gravity model, we evolve a magnetized disk using a modern general relativistic magnetohydrodynamics code. We will show that many aspects of the disk follow the binary inward as its separation diminishes up until when the binary shrinkage timescale becomes smaller than the inflow timescale at the inner edge of the disk. We will also present predictions for the bolometric luminosity using our radiative cooling function as a proxy for emissivity.

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