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X-rays From Centrifugal Magnetospheres in Massive Stars

Published online by Cambridge University Press:  23 January 2015

Christopher Bard  and
Richard Townsend
Christopher Bard*
Affiliation:
University of Wisconsin, Madison
Richard Townsend
Affiliation:
University of Wisconsin, Madison
*
Corresponding email: bard@astro.wisc.edu
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Abstract

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In the subset of massive OB stars with strong global magnetic fields, X-rays arise from magnetically confined wind shocks (Babel & Montmerle 1997). However, it is not yet clear what the effect of stellar rotation and mass-loss rate is on these wind shocks and resulting X-rays. Here, we present results from a grid of Arbitrary Rigid-Field Hydrodynamic simulations (ARFHD) of a B-star centrifugal magnetosphere with an eye towards quantifying the effect of stellar rotation and mass-loss rate on the level of X-ray emission. The results are also compared to a generalized XADM model for X-rays in dynamical magnetospheres (ud-Doula et al. 2014).

References

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