Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...20111301t&link_type=abstract
American Astronomical Society, 201st AAS Meeting, #113.01; Bulletin of the American Astronomical Society, Vol. 34, p.1284
Astronomy and Astrophysics
Astronomy
3
Scientific paper
With the discovery of a strong magnetic field on θ 1 Orionis C, the magnetically confined wind shock model has become a leading explanation for X-ray emission from some O and B stars. This model involves a dipole field that channels the stellar wind from both poles of the star towards the equator where the resulting shocks heat the wind to X-ray emitting temperatures. As the shocked wind cools, it feeds an equatorial disk that can be opaque to X-rays. In this poster we describe synthetic line profiles from both analytic models and magnetohydrodynamic numerical simulations of magnetically confined hot star winds. We discuss the effect of the closed vs. open field regions on line shape and width, and also discuss effects of absorption arising from the equatorial cooling disk and the cool polar wind. For a star with a tilted dipole, our viewing angle to the magnetically confined wind structure changes as the star rotates, making the line profiles phase-dependent. We compare our synthesized line profiles and band-pass fluxes to phase-resolved Chandra spectra of θ 1 Orionis C. This work is supported by the NASA, under grant NAS8-39073.
Cohen David H.
Gagne Marc
Oksala Mary
Owocki Stanley P.
Tonnesen Stephanie K.
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