Spectral line signatures of relativistic disks

Details Spectral line signatures of relativistic disks Spectral line signatures of relativistic disks

Apr 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aipc..431..265r&link_type=abstract

Accretion processes in astrophysical systems: Some like it hot! - eigth astrophysics conference. AIP Conference Proceedings, Vo

Astronomy and Astrophysics

Astrophysics

1

Radiative Transfer, Scattering, Black Holes, Infall, Accretion, And Accretion Disks, Active And Peculiar Galaxies And Related Systems

Scientific paper

We consider emission line formation in a thin accretion disk around a black hole, taking into account the differential flow of material in the disk. If the disk is optically thick in the line, local velocity gradients can cause the integrated intensity to have azimuthal dependence in the emitter frame. We examine this effect with simple parameterized models based on Sobolev theory to highlight the overall character of the changes in the observed line profile. The shape of the profile, which can serve as a diagnostic of the disk geometry and the spin of the black hole, may be significantly altered by the velocity-gradient effect. Specifically, we find that the effect causes a decrease of flux in the blue Doppler peak, which in turn would lead to an underestimate of the inner disk radius. If the inner radius were used as a signature of black hole rotation, as when the disk is not emissive within the marginally stable circular orbit, then the inferred rotation would be overestimated in cases where the emissivity of the disk has fairly shallow fall-off with radius. If the disk were emissive even within the marginally stable orbit, then the local azimuthal anisotropy of emission could produce features in the line profile which distinguish rotating from nonrotating black holes.

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