Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...390..645m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 390, no. 2, May 10, 1992, p. 645-649.
Astronomy and Astrophysics
Astrophysics
2
Accretion Disks, Mass Transfer, Stellar Mass Ejection, X Ray Stars, Companion Stars, Hadrons, Neutrinos, Stellar Orbits
Scientific paper
The contention that the high-energy neutrinos likely to be produced in the body of the companion in Cygnus X - 3 as a result of the emission of ultrahigh-energy hadrons from the compact body may heat and inflate the companion is discussed. For reasonable approximations, the inflated companion can yield mass transfer on a scale equal to the observed orbital lengthening time scale of about 100,000 yr by continuing to nearly fill its lobe. This kind of mass transfer can be supplemented by a self-excited wind due to X-rays, gamma-rays, or the hadron beam. The former mode of mass transfer appears to be a necessity because if the latter model operates alone it is likely to lead to quenching of the central accretion engine or a runaway mass transfer in Cygnus X - 3. For a sufficiently neutrino-opaque companion, a modest value of hadron beam power of 10 exp 37 ergs/s can generate a marginally super Eddington mass loss rate of greater than about 10 exp 18 g/s for a companion mass of greater than about 0.01 solar mass.
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