On the Accretion Instability in Soft X-Ray Transients

Details On the Accretion Instability in Soft X-Ray Transients On the Accretion Instability in Soft X-Ray Transients

Jun 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...464l.139v&link_type=abstract

Astrophysical Journal Letters v.464, p.L139

Astronomy and Astrophysics

Astronomy

215

Accretion, Accretion Disks, X-Rays: General

Scientific paper

Dwarf nova outbursts are likely caused by a thermal-viscous instability in the accretion disk around the white dwarf, which can occur if the mass transfer rate, M dot , is below a critical value (which depends on orbital period). Based on data for soft X-ray transients and persistent low-mass X-ray binaries with known distances and orbital periods, Porb, I show that for these systems the distributions in a (Porb, M dot ) diagram can be understood with the dwarf nova instability criterion, if that is adapted to include X-ray heating of the disk. This supports the idea that the disk instability model applies to soft X-ray transients, and shows that X-ray heating must be included in modeling the outbursts.

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