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M. Oksala, M. Gagne (West Chester University), D. Cohen, S. Tonnesen (Swarthmore College), A. ud-Doula (North Caroline State University), S. Owocki (Bartol Research Institute), J. MacFarlane (Prism Computational Sciences)
Chandra High-Energy Grating spectra obtained at four rotational phases of \theta1 Ori C (O6-7 V), corresponding to four different viewing angles with respect to the magnetic axis, are used to constrain the temperature, spatial location, and kinematics of the hot plasma on this very young hot star with a strong (1100 G) dipole field. The plasma is moving, but only at speeds of a few 100 km s-1, much slower than the terminal wind velocity. It is close to the star (within 1.5 R* of the surface) and hot (peak temperature ~30 MK). We analyze these diagnostics in conjunction with new MHD simulations of the magnetically channeled wind shock mechanism on \theta1 Ori C. This model fits all the data surprisingly well, reproducing the very high temperatures, relatively narrow and unshifted lines, and the near-star source location.
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Bulletin of the American Astronomical Society, 36 #2
© YEAR. The American Astronomical Soceity.