The Wind-Wind Collision Region of the Wolf-Rayet Binary V444 Cyg: How much optical line emission does it produce ?

Details The Wind-Wind Collision Region of the Wolf-Rayet Binary V444 Cyg: How much optical line emission does it produce ? The Wind-Wind Collision Region of the Wolf-Rayet Binary V444 Cyg: How much optical line emission does it produce ?

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...19915506f&link_type=abstract

American Astronomical Society, 199th AAS Meeting, #155.06; Bulletin of the American Astronomical Society, Vol. 34, p.562

Astronomy and Astrophysics

Astronomy

Scientific paper

We model the emission line profile variations that are expected to be produced by physical and wind eclipses in the Wolf-Rayet (WR+O) binary system V444 Cyg. A comparison of the theoretical profiles with the He II 4686 Å line observed in V444 Cyg allows us to isolate the effects that are likely to be due to the wind-wind collision region, in this particular line. We estimate that the WWC region contributes no more than ~ 12% of the equivalent width of the emission line, with smaller values during elongations, when part of the shock cone is being eclipsed by the O-star. The upper limit implies a maximum contribution from the wind-wind collision region of ~ 1.*E35 ergs s-1 to the total luminosity of He II 4686 Å line. Using the analytical solution of Cantó et al. (1996), we find that the bulk of this emission seems to be arising along the shock cone walls where the flow velocity is ~ 800 km s-1, at a distance of ~ 8 {Rsun }\> from the O-star's surface, and at Θ =60-70o from the line joining the centers of the two stars, with origin in the O-star. The derived surface density of this region is σ =0.22 gr cm-2, which together with the He II 4686 Å luminosity, indicates that the thickness of the shock lies in the range 2-10 x 1010 cm and the total density is 1-6 x 1012 cm-3.

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