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Rigid Field Hydrodynamic simulations of the magnetosphere of σ Orionis E

Published online by Cambridge University Press:  12 July 2011

Nicholas R. Hill ,
Richard H. D. Townsend ,
David H. Cohen  and
Marc Gagné
Nicholas R. Hill
Affiliation:
Dept. of Astronomy, University of Wisconsin-Madison, Madison, WI 53706, USA
Richard H. D. Townsend
Affiliation:
Dept. of Astronomy, University of Wisconsin-Madison, Madison, WI 53706, USA
David H. Cohen
Affiliation:
Dept. of Physics and Astronomy, Swarthmore College, Swarthmore, PA 19081, USA
Marc Gagné
Affiliation:
Dept. of Geology and Astronomy, West Chester University, West Chester, PA 19383, USA
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Abstract

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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.

Keywords

hydrodynamicsstars: magnetic fieldsstars: mass lossX-rays: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 194 - 195
Copyright
Copyright © International Astronomical Union 2011

References

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