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2007MNRAS.382..139T - Mon. Not. R. Astron. Soc., 382, 139-157 (2007/November-3)
A rigid-field hydrodynamics approach to modelling the magnetospheres of massive stars.
TOWNSEND R.H.D., OWOCKI S.P. and UD-DOULA A.
Abstract (from CDS):
The simulations confirm many of the predictions of previous analytical and numerical studies. Collisions between wind streams from opposing magnetic hemispheres lead to strong shock heating. The post-shock plasma cools initially via X-ray emission, and eventually accumulates into a warped, rigidly rotating disc defined by the locus of minima of the effective (gravitational plus centrifugal) potential. However, a number of novel results also emerge. For field lines extending far from the star, the rapid area divergence enhances the radiative acceleration of the wind, resulting in high shock velocities (up to ∼3000km/s) and hard X-rays. Moreover, the release of centrifugal potential energy continues to heat the wind plasma after the shocks, up to temperatures around twice those achieved at the shocks themselves. Finally, in some circumstances the cool plasma in the accumulating disc can oscillate about its equilibrium position, possibly due to radiative cooling instabilities in the adjacent post-shock regions.
Abstract Copyright: 2007 The Authors. Journal compilation © 2007 RAS
Journal keyword(s): hydrodynamics - stars: magnetic fields - stars: mass-loss - stars: rotation - gamma-rays: theory - X-rays: stars
Simbad objects: 5
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