Rigid Field Hydrodynamic simulations of the magnetosphere of σ Orionis E

Type Conference Paper
Names Nicholas R. Hill, Richard H. D. Townsend, David H. Cohen, Marc Gagné
Conference Name IAU Symposium
Volume 272
Pages 194-195
Date July 1, 2011
DOI 10.1017/S1743921311010301
ISBN 1743-9221
URL http://adsabs.harvard.edu/abs/2011IAUS..272..194H
Library Catalog NASA ADS
Abstract We present Rigid Field Hydrodynamic simulations of the magnetosphere of σ Ori E. We find that the X-ray emission from the star's magnetically confined wind shocks is very sensitive to the assumed mass-loss rate. To compare the simulations against the measured X-ray emission, we first disentangle the star from its recently discovered late-type companion using Chandra HRC-I observations. This then allows us to place an upper limit on the mass-loss rate of the primary, which we find to be significantly smaller than previously imagined.
Tags Stars: Mass Loss, X-rays: stars, hydrodynamics, stars: magnetic fields
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