Accretion-disk scenarios of the precursor peak in X-ray transients

Details Accretion-disk scenarios of the precursor peak in X-ray transients Accretion-disk scenarios of the precursor peak in X-ray transients

May 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976natur.261..211s&link_type=abstract

Nature, vol. 261, May 20, 1976, p. 211-213.

Astronomy and Astrophysics

Astronomy

6

Astronomical Models, Stellar Structure, X Ray Sources, Black Holes (Astronomy), Neutron Stars, Roche Limit, Stellar Luminosity, Thermal Instability, X Ray Spectra

Scientific paper

Three schemes are presented which provide qualitative explanations of the precursor peak and related phenomena of transient X-ray sources on the basis of accretion-disk behavior with a rising accretion rate (M), followed by its gradual subsidence and the emptying of the disk. In the first, Roche-lobe overflow begins and increases and a disk forms. Initially, very soft X-ray flux from portions of the disk with large radii dominate, but luminosity in the 1-20 keV range becomes significant as a stable type II inner region develops. The continuing rise in M leads to an increasing luminosity; as M begins to decrease, the transient enters its decay phase. The second, pertaining to non-magnetic situations, black holes or neutron stars, begins and ends like the first. However, in the rise to the precursor peak with increasing M an unstable radiation dominated inner region appears or thermal instabilities develop from severe density thinning across the inner edge, and the inner region blows up into a very hot, spherical cloud. The third scenario applies only to a black hole in a stellar wind environment and requires an increasing M and increasing angular momentum of the accreting material. An initial accretion disk is formed at very small radii and grows into a stable disk. The disk evolution is described in terms of the orbital topography of the Schwarzschild metric.

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