ROSAT X-ray observations of the WR stars HD 50896 (WN5) and gamma Velorum (WC8+O9I)

Details ROSAT X-ray observations of the WR stars HD 50896 (WN5) and gamma Velorum (WC8+O9I) ROSAT X-ray observations of the WR stars HD 50896 (WN5) and gamma Velorum (WC8+O9I)

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ap%26ss.221..321w&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 221, no. 1-2, p. 321-331

Astronomy and Astrophysics

Astronomy

1

Spaceborne Astronomy, Spectrum Analysis, Stellar Physics, Stellar Systems, Stellar Winds, Wolf-Rayet Stars, X Ray Astronomy, X Ray Spectra, X Ray Stars, Brightness, Data Processing, Data Reduction, Heao 2, Rosat Mission, Shock Waves, Stellar Luminosity

Scientific paper

We present a preliminary analysis of multiple X-ray (0.1-2.5 keV) observations of HD 50896 and gamma Velorum obtained with the ROSAT satellite. For HD 50896, our 8 observations show variability at the 30% level on timescales of approximately 1 day, together with larger (x 1.7) epoch-changes, but no evidence for rapid variability. No phase-dependent modulation is apparent on the 3.766 d optical period. The mean Position Sensitive Proportional Counter (PSPC) spectrum gives kT = 0.28 kev, log N(H) = 20.6, and Lx = 3.8 x 1032 erg/s, and implies that the observed X-rays have undergone little absorption in the WN5 wind. For gamma Velorum, we have 13 observations secured over several cycles in the 78.5 d binary period. At most binary phases, the X-ray emission is relatively constant, with kT approximately equal to 0.19 keV, log N(H) = 20.2, and Lx = 2.5 x 1031 erg/s. Near orbital phase 0.5, the X-ray emission is enhanced by a factor of 4, due almost entirely to an additional harder component with kT greater than 2 keV. We believe this is due to X-ray emission produced in the collision of the two stellar winds.

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