X-ray Polarization from Accreting Black Holes: II. The Thermal State

Details X-ray Polarization from Accreting Black Holes: II. The Thermal State X-ray Polarization from Accreting Black Holes: II. The Thermal State

2009-02-23

arxiv.org/abs/0902.3982v1

Astrophys.J.701:1175-1187,2009

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

33 pages, 13 figures, submitted to ApJ

Scientific paper

10.1088/0004-637X/701/2/1175

We present new calculations of X-ray polarization from black hole (BH) accretion disks in the thermally-dominated state, using a Monte-Carlo ray-tracing code in full general relativity. In contrast to many previously published studies, our approach allows us to include returning radiation that is deflected by the strong-field gravity of the BH and scatters off of the disk before reaching a distant observer. Although carrying a relatively small fraction of the total observed flux, the scattered radiation tends to be highly polarized and in a direction perpendicular to the direct radiation. For moderately large spin parameters (a/M >~ 0.9), this scattered returning radiation dominates the polarization signal at energies above the thermal peak, giving a net rotation in the polarization angle of 90 deg. We show how these new features of the polarization spectra from BHs in the thermal state may be developed into a powerful tool for measuring BH spin and probing the gas flow in the innermost disk. In addition to determining the emission profile, polarization observations can be used to constrain other properties of the system such as BH mass, inclination, and distance. New instruments currently under development should be able to exploit this tool in the near future.

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