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Title:
A rigidly rotating magnetosphere model for circumstellar emission from magnetic OB stars
Authors:
Townsend, R. H. D.; Owocki, S. P.
Affiliation:
AA(Bartol Research Institute, University of Delaware, Newark, DE 19716, USA; Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT), AB(Bartol Research Institute, University of Delaware, Newark, DE 19716, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 357, Issue 1, pp. 251-264. (MNRAS Homepage)
Publication Date:
02/2005
Origin:
MNRAS
MNRAS Keywords:
stars: chemically peculiar, stars: early-type, stars: emission-line, Be, stars: magnetic fields, stars: mass-loss, stars: rotation
DOI:
10.1111/j.1365-2966.2005.08642.x
Bibliographic Code:
2005MNRAS.357..251T

Abstract

We present a semi-analytical approach for modelling circumstellar emission from rotating hot stars with a strong dipole magnetic field tilted at an arbitrary angle to the rotation axis. By assuming the rigid-field limit in which material driven (e.g. in a wind outflow) from the star is forced to remain in strict rigid-body corotation, we are able to solve for the effective centrifugal-plus-gravitational potential along each field line, and thereby identify the location of potential minima where material is prone to accumulate. Applying basic scalings for the surface mass flux of a radiatively driven stellar wind, we calculate the circumstellar density distribution that obtains once ejected plasma settles into hydrostatic stratification along field lines. The resulting accumulation surface resembles a rigidly rotating, warped disc, tilted such that its average surface normal lies between the rotation and magnetic axes. Using a simple model of the plasma emissivity, we calculate time-resolved synthetic line spectra for the disc. Initial comparisons show an encouraging level of correspondence with the observed rotational phase variations of Balmer-line emission profiles from magnetic Bp stars such as σ Ori E.

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