A first detailed study of the colliding wind WR+O binary WR 30a

Details A first detailed study of the colliding wind WR+O binary WR 30a A first detailed study of the colliding wind WR+O binary WR 30a

Oct 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001mnras.327..435g&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 327, Issue 2, pp. 435-451.

Astronomy and Astrophysics

Astronomy

33

Binaries: Spectroscopic, Stars: Individual: Wr 30A, Stars: Mass-Loss, Stars: Wolf-Rayet

Scientific paper

We present a detailed, extensive investigation of the photometric and spectroscopic behaviour of WR 30a. This star is definitely a binary system with a period around 4.6d. We propose the value P=4.619d (σ=0.002d). The identification of the components as WO4+O5((f)) indicates a massive evolved binary system; the O5 component is a main-sequence or, more likely, a giant star. The radial velocities of the O star yield a circular orbit with an amplitude KO=29.9 (σ=2.1)kms-1 and a mass function of 0.013 (σ=0.003)Msolar. The spectrum of WR 30a exhibits strong profile variations of the broad emission lines that are phase-locked with the orbital period. We report the detection of the orbital motion of the WO component with KWO=189kms-1, but this should be confirmed by further observations. If correct, it implies a mass ratio MWO /MO=0.16. The star exhibits sinusoidal light variations of amplitude 0.024mag peak-to-peak with the minimum of light occurring slightly after the conjunction with the O star in front. On the basis of the phase-locked profile variations of the Civ λ4658 blend in the spectrum of the WO, we conclude that a wind-wind collision phenomenon is present in the system. We discuss some possibilities for the geometry of the interaction region.

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