X-ray Line Profile Signatures of a Bardeen-Petterson Disk Around a Rotating Black Hole

Details X-ray Line Profile Signatures of a Bardeen-Petterson Disk Around a Rotating Black Hole X-ray Line Profile Signatures of a Bardeen-Petterson Disk Around a Rotating Black Hole

Nov 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..ses.hd007m&link_type=abstract

American Physical Society, 71st Annual Meeting of the Southeastern Section, 11-13 November, 2004, Oak Ridge, TN. MEETING ID: S

Physics

Scientific paper

Broadened emission lines have been observed in the X-ray spectra of over a dozen Seyfert-1 galaxies. More recently similar features have also been discovered in Galactic black holes and black hole candidates. These lines, from fluorescent K-alpha emission of cold iron (ionization states less than Fe XVII), provide a unique diagnostic of the inner regions of accretion flows around black holes. Since the line energy is well known (6.40 keV) and its intrinsic width is very small, the observed, broadened line profile can provide direct information on the Doppler shifts and gravitational redshifts affecting the line-emitting material, and are sensitive to features of realistic disk models such as turbulent broadening and radial inflow. The dependence of these line profiles on disk radii and inclination angle suggest that they may be useful as a diagnostic of warped or tilted accretion disks, and perhaps relevant to the galactic microquasar V4641. For a thin disk tilted with respect to the midplane of the black hole, the Lense-Thirring precession will cause the disk to warp. In disks with efficient angular momentum transport, the misaligned angular momentum can propagate out to large radii leaving the inner region of the disk aligned with the midplane of the black hole - the Bardeen-Petterson effect. We examine possible signatures of Pardeen-Petterson disks in X-ray line profiles by numerically generating the profiles using a ray-tracing code on the stationary spacetime geometry of a spinning black hole.

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