Spectroscopic study of the short-period WN5o + O8.5V binary system WR127 (HD 186943)

Details Spectroscopic study of the short-period WN5o + O8.5V binary system WR127 (HD 186943) Spectroscopic study of the short-period WN5o + O8.5V binary system WR127 (HD 186943)

Feb 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011mnras.411..635d&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 411, Issue 1, pp. 635-643.

Astronomy and Astrophysics

Astronomy

1

Techniques: Spectroscopic, Binaries: Spectroscopic, Stars: Individual: Wr127, Stars: Mass-Loss, Stars: Winds, Outflows, Stars: Wolf-Rayet

Scientific paper

Combined with previous information (orbital period P= 9.5550 d and inclination ?), new optical spectroscopic data lead to improved circular orbits for this WR + O system, with mass 13.4 M&sun; of the WN5o star and 23.9 M&sun; of its O8.5V companion. These are normal for their spectral types. The WR/O mass ratio, q≃ 0.56, is reasonable for such a binary. The relatively large orbital separation between the two components (˜63 R&sun;) implies that there is currently no interaction between the two stars beyond their colliding winds. Analysis of the excess line emission and absorption arising in the wind-wind collision zone yields the following parameters: streaming velocity vstrm= 1104 km s-1, cone opening half-angle θ≃ 59° and Coriolis angle shift ?. Using probable values of mass-loss rate and terminal wind velocity for each star, a value of θ≃ 37° is obtained. The difference in θ is likely due to a combination of uncertainty in these parameters and radiative braking. Altogether, WR127 is a normal, detached and non-photospherically eclipsing binary system, although it does show atmospheric ‘eclipses'.

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