Journal
ASTROPHYSICAL JOURNAL
Volume 530, Issue 1, Pages L25-L28Publisher
UNIV CHICAGO PRESS
DOI: 10.1086/312475
Keywords
accretion, accretion disks; binaries : close; stars : individual (SS 433); X-rays : stars
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We consider possible evolutionary models for SS 433. We assume that common envelope evolution is avoided if radiation pressure is able to expel most of a super-Eddington accretion flow from a region smaller than the accretor's Roche lobe. This condition is satisfied, at least initially, for largely radiative donors with masses in the range 4-12 M.. For donors more massive than about 5 M., moderate mass ratios q = M-2/M-1 greater than or similar to 1 are indicated, thus tending to favor black hole accretors. For lower mass donors, evolutionary considerations do not distinguish between a neutron star or black hole accretor. In all cases the mass transfer (and mass-loss) rates M-tr similar to 7 x 10(-6) to 4 x 10(-4) M, yr(-1) are much larger than the likely mass-loss rate M-jet similar to 10(-6) M. yr(-1) in the precessing jets. Almost all of the transferred mass is expelled at radii considerably larger than the jet acceleration region, producing the stationary H alpha line and the infrared luminosity and accounting for the low X-ray luminosity.
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