Quiescent accretion disks in black hole X-ray novae

Details Quiescent accretion disks in black hole X-ray novae Quiescent accretion disks in black hole X-ray novae

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...436..848o&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 436, no. 2, p. 848-858

Astronomy and Astrophysics

Astronomy

70

Accretion Disks, Balmer Series, Black Holes (Astronomy), Novae, Stellar Mass Accretion, Stellar Models, Stellar Spectra, X Ray Binaries, Astronomical Spectroscopy, H Alpha Line, Mathematical Models

Scientific paper

We present detailed time-resolved spectroscopy of the Balmer emission lines from two black hole binary systems in quiescence, A0620-00 and Nova Muscae 1991. We find extraordinary similarities between the two systems. There are 30-40 km/s velocity variations of the emission lines over the orbital period, the phases of which are not aligned with the expected phase of the motion of the compact primary. Detailed modeling of both systems is complicated by variable hot spot components, regions of optical thickness, and intermittent excess emission in the blue line wings of the H-alpha lines. Both sources also display low velocities at the outer edge of the accretion disk, implying a large primary Roche lobe and extreme mass ratios. These complications suggest that although simple optically thin, Keplerian alpha-disk models provide a useful parameterization of emission lines from these systems, the straightforward physical models they imply should be treated with great caution.

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