On the Periodic X-Ray Emission from the O7 V Star theta 1 Orionis C

Astronomy and Astrophysics – Astronomy

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Stars: Individual Constellation Name: Theta 1 Orionis C, Stars: Early-Type, Stars: Magnetic Fields, Stars: Mass Loss, X-Rays: Stars

Scientific paper

The O7 V star theta 1 Orionis C was very recently found to present a strong periodic variation of the X-ray emission (Gagne et al. 1997) that is in agreement with the period determined from the variability of spectral lines (Stahl et al. 1996). The authors suggested that the variations are caused by an oblique magnetic rotator with a large-scale magnetic field modulating the wind. We present here the hypothesis of a dipolar magnetic field embedded in the radiation-driven wind of theta 1 Orionis C and analyze the X-ray data in the framework of the magnetically confined wind shock (MCWS) model (Babel & Montmerle 1997). We find that both the ROSAT HRI count rate and the periodic variability of theta 1 Orionis C are quantitatively reproduced by the model, provided that the field has an intensity at the stellar surface of B* ~= 300 G. The variability is caused in large part by the circumstellar cooling disk predicted by the MCWS model. These results give strong support to a magnetic origin for the variability of theta 1 Orionis C and render this star the best candidate for a high-mass analog to magnetic Bp stars.

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