SS 433: a WR X-ray binary or a WR-type phenomenon ?

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dc.creatorFuchs, Yael
dc.creatorMiramond, L. Koch
dc.creatorAbraham, P.
dc.date2004-10-20
dc.date.accessioned2026-07-07T02:15:24Z
dc.date.available2026-07-07T02:15:24Z
dc.descriptionWe present mid-infrared spectra of the microquasar SS 433 obtained with the Infrared Space Observatory (spectroscopic mode of ISOPHOT) and compare them to the spectra of four Wolf-Rayet stars. The mid-infrared spectrum of SS 433 shows mainly HI and HeI emission lines and is very similar to the spectrum of WR 147, a WN8(h)+B0.5V binary with a colliding wind. The 2-12 micron continuum emission corresponds to optically thin and partially optically thick free-free emission from which we calculate a mass loss rate of 1.4-2.2x10^{-4} M_sun/yr if the wind is homogeneous and a third of these values if it is clumped, which is consistent with a strong WN stellar wind. We propose that this strong wind outflows from a geometrically thick envelope of material surrounding the compact object like a stellar atmosphere, imitating the Wolf-Rayet phenomenon.
dc.description5 pages, 2 ps figure files, to appear in proceedings of "Massive Stars in Interacting Binaries" (Lac Sacacomie, Quebec, 16-20 Aug 2004) eds. Nicole St-Louis & Tony Moffat, ASP Conference Series
dc.identifierhttps://arxiv.org/abs/astro-ph/0410480
dc.identifierhttp://arxiv.org/abs/astro-ph/0410480
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/8397
dc.subjectAstrophysics
dc.titleSS 433: a WR X-ray binary or a WR-type phenomenon ?
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