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2002MNRAS.333...55D - Mon. Not. R. Astron. Soc., 333, 55-70 (2002/June-2)
The magnetic field and wind confinement of θ 1 Orionis C.
DONATI J.-F., BABEL J., HARRIES T.J., HOWARTH I.D., PETIT P. and SEMEL M.
Abstract (from CDS):
We also investigate in this paper the magnetic confinement of the radiatively driven wind of θ1 Ori C in the context of the magnetically confined wind-shock model of Babel & Montmerle. In the case of θ1 Ori C, this model predicts the formation of a large magnetosphere (extending as far as 2-3R ∗), consisting of a very hot post-shock region (with temperatures in excess of 10MK and densities of about 1010-1011 cm–3) generated by the strong collision of the wind streams from both stellar magnetic hemispheres, as well as a dense cooling disc forming in the magnetospheric equator. We find that this model includes most of the physics required to obtain a satisfactory level of agreement with the extensive data sets available for θ1 Ori C in the literature (and, in particular, with the recent X-ray data and the phase-resolved spectroscopic observations of ultraviolet and optical wind lines) provided that the mass-loss rate of θ1 Ori C is at least 5 times smaller than that predicted by radiatively driven wind models. We finally show how new observations with the XMM or Chandra spacecraft could help us constrain this model much more tightly and thus obtain a clear picture of how magnetic fields can influence the winds of hot stars.
Abstract Copyright: 2002 Blackwell Science Ltd
Journal keyword(s): stars: individual: θ1 Ori C - stars: magnetic fields - stars: rotation - stars: winds, outflows
Simbad objects: 4
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