The evolutionary status of SS 433

Andrew R. King; Ronald E. Taam; Mitchell C. Begelman

doi:10.1086/312475

The evolutionary status of SS 433

Andrew R. King^*, Ronald E. Taam, Mitchell C. Begelman

^*Corresponding author for this work

Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

61 Scopus citations

Abstract

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 = M₂/M₁ ≳ 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_lr ∼ 7 × 10^-6 to 4 × 10^-4 M_⊙ yr^-1 are much larger than the likely mass-loss rate M_jet ∼ 10^-6 M_⊙ yr^-1 in the processing jets. Almost all of the transferred mass is expelled at radii considerably larger than the jet acceleration region, producing the "stationary" Hα line and the infrared luminosity and accounting for the low X-ray luminosity.

Original language	English (US)
Pages (from-to)	L25-L28
Journal	Astrophysical Journal
Volume	530
Issue number	1 PART 2
DOIs	https://doi.org/10.1086/312475
State	Published - Feb 10 2000

Funding

This research was begun at the Institute for Theoretical Physics and supported in part by the National Science Foundation under grant number PHY 94-07194. A. R. K. gratefully acknowledges support by the UK Particle Physics and Astronomy Research Council through a Senior Fellowship. R. T. acknowledges support from NSF grant AST 97-27875. M. C. B. acknowledges support from NSF grants AST 95-29170 and AST 98-76887 and a Guggenheim Fellowship.

Keywords

Accretion, accretion disks
Binaries: Close
Stars: Individual (SS 433)
X-rays: Stars

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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title = "The evolutionary status of SS 433",

abstract = "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 = M2/M1 ≳ 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 Mlr ∼ 7 × 10-6 to 4 × 10-4 M⊙ yr-1 are much larger than the likely mass-loss rate Mjet ∼ 10-6 M⊙ yr-1 in the processing jets. Almost all of the transferred mass is expelled at radii considerably larger than the jet acceleration region, producing the {"}stationary{"} Hα line and the infrared luminosity and accounting for the low X-ray luminosity.",

keywords = "Accretion, accretion disks, Binaries: Close, Stars: Individual (SS 433), X-rays: Stars",

author = "King, {Andrew R.} and Taam, {Ronald E.} and Begelman, {Mitchell C.}",

note = "Funding Information: This research was begun at the Institute for Theoretical Physics and supported in part by the National Science Foundation under grant number PHY 94-07194. A. R. K. gratefully acknowledges support by the UK Particle Physics and Astronomy Research Council through a Senior Fellowship. R. T. acknowledges support from NSF grant AST 97-27875. M. C. B. acknowledges support from NSF grants AST 95-29170 and AST 98-76887 and a Guggenheim Fellowship.",

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AU - Begelman, Mitchell C.

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N2 - 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 = M2/M1 ≳ 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 Mlr ∼ 7 × 10-6 to 4 × 10-4 M⊙ yr-1 are much larger than the likely mass-loss rate Mjet ∼ 10-6 M⊙ yr-1 in the processing jets. Almost all of the transferred mass is expelled at radii considerably larger than the jet acceleration region, producing the "stationary" Hα line and the infrared luminosity and accounting for the low X-ray luminosity.

AB - 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 = M2/M1 ≳ 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 Mlr ∼ 7 × 10-6 to 4 × 10-4 M⊙ yr-1 are much larger than the likely mass-loss rate Mjet ∼ 10-6 M⊙ yr-1 in the processing jets. Almost all of the transferred mass is expelled at radii considerably larger than the jet acceleration region, producing the "stationary" Hα line and the infrared luminosity and accounting for the low X-ray luminosity.

KW - Accretion, accretion disks

KW - Binaries: Close

KW - Stars: Individual (SS 433)

KW - X-rays: Stars

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ER -

The evolutionary status of SS 433

Abstract

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