Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...162...71h&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 162, no. 1-2, July 1986, p. 71-79.
Astronomy and Astrophysics
Astrophysics
109
Red Dwarf Stars, Stellar Models, X Ray Binaries, Accretion Disks, Mass Flow Rate, Stellar Atmospheres, Stellar Envelopes, Stellar Mass Accretion
Scientific paper
The existing database on the physical characteristics of stellar soft and ultrasoft transient X-ray bursts is summarized in order to form a generic model for the sources. The bursts have come from binary systems which repeat the bursts with a frequency of about a year. Bursts possess energies of about 10 to the 44th ergs emitted for months and reaching maximum luminosities of 10 to the 37th to 10 to the 38th ergs, levels associated with an accretion rate of 10 billion grams/sec. The transients are shown to arise because of a mass loss instability in the secondary star, believed to be red dwarf. Analysis of the structure of the envelope of a dwarf heated by X-rays shows that subphotospheric layers can expand during the quiescent phase and enter into a mass transfer instability condition near the Roche lobe. The accretion disk eventually blocks the X-ray input and the transfer to the primary, a neutron star, abates.
Hameury Jean-Marie
King Andrew R.
Lasota Jean-Pierre
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