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First 3DMHD simulation of a massive-star magnetosphere with application to Hα emission from θ<SUP>1</SUP> Ori C
ud-Doula, A. ( Penn State Worthington Scranton, Dunmore, PA 18512, USA; ); Sundqvist, J. O. ( Bartol Research Institute, University of Delaware, Newark, DE 19716, USA ); Owocki, S. P. ( Bartol Research Institute, University of Delaware, Newark, DE 19716, USA ); Petit, V. ( Department of Geology and Astronomy, West Chester University, West Chester, PA 19383, USA ); Townsend, R. H. D. ( Department of Astronomy, University of Wisconsin-Madison, 5534 Sterling Hall, 475 N Charter Street, Madison, WI 53706, USA ) show affiliations
Monthly Notices of the Royal Astronomical Society, Volume 428, Issue 3, p.2723-2730
Published in Jan 2013
We present the first fully 3D magnetohydrodynamic (MHD) simulation for magnetic channelling and confinement of a radiatively driven, massive-star wind. The specific parameters are chosen to represent the prototypical slowly rotating magnetic O star θ1 Ori C, for which centrifugal and other dynamical effects of rotation are negligible. The computed global structure in latitude and radius resembles that found in previous 2D simulations, with unimpeded outflow along open field lines near the magnetic poles, and a complex equatorial belt of inner wind trapping by closed loops near the stellar surface, giving way to outflow above the Alfvén radius. In contrast to this previous 2D work, the 3D simulation described here now also shows how this complex structure fragments in azimuth, forming distinct clumps of closed loop infall within the Alfvén radius, transitioning in the outer wind to radial spokes of enhanced density with characteristic azimuthal separation of 15°-20°. Applying these results in a 3D code for line radiative transfer, we show that emission from the associated 3D `dynamical magnetosphere' matches well the observed Hα emission seen from θ1 Ori C, fitting both its dynamic spectrum over rotational phase and the observed level of cycle-to-cycle stochastic variation. Comparison with previously developed 2D models for the Balmer emission from a dynamical magnetosphere generally confirms that time averaging over 2D snapshots can be a good proxy for the spatial averaging over 3D azimuthal wind structure. Nevertheless, fully 3D simulations will still be needed to model the emission from magnetospheres with non-dipole field components, such as suggested by asymmetric features seen in the Hα equivalent-width curve of θ1 Ori C.
Astronomy: MHD; magnetic fields; outflows; stars: early-type; stars: mass-loss; stars: rotation; stars: winds
arXiv: Astrophysics - Solar and Stellar Astrophysics
2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society