X-rays From Centrifugal Magnetospheres in Massive Stars
Abstract
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).
- Publication:
-
New Windows on Massive Stars
- Pub Date:
- January 2015
- DOI:
- 10.1017/S1743921314007352
- Bibcode:
- 2015IAUS..307..449B