Precession of Accretion Disks in X-Ray Binaries

Details Precession of Accretion Disks in X-Ray Binaries Precession of Accretion Disks in X-Ray Binaries

Dec 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...18710408i&link_type=abstract

American Astronomical Society, 187th AAS Meeting, #104.08; Bulletin of the American Astronomical Society, Vol. 27, p.1435

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Scientific paper

An increasing number of stellar close Binary systems, especially X-Ray Binaries is found to display a "long-term periodicity" with a period which is typically one to two orders of magnitude larger than the system's binary period. Nearly all massive X-ray binaries may turn out to have a long-term period, caused by a regular feature, common to all X-ray binaries. It is argued that the possession of an accretion disk, which precesses, driven by tidal interaction, is the most likely candidate for the long-term periodicity. If one assumes tidal interaction responsible for the precession, systems with a known long-term periodicity allow an independent estimate for the mass at the center of the accretion disk. It is indeed possible to make a crude independent estimate of the mass at the center of the disk if one assumes disk-precession driven tidally. This independent mass estimate indicates a massive blackhole for CygX-1. However other causes for long-term periods in X-ray binaries, such as the dot {M} variations remain possible.

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