Rigid Field Hydrodynamic simulations of the magnetosphere of σ Orionis E

Details Rigid Field Hydrodynamic simulations of the magnetosphere of σ Orionis E Rigid Field Hydrodynamic simulations of the magnetosphere of σ Orionis E

Jul 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..272..194h&link_type=abstract

Active OB stars: structure, evolution, mass loss, and critical limits, Proceedings of the International Astronomical Union, IAU

Astronomy and Astrophysics

Astronomy

1

Hydrodynamics, Stars: Magnetic Fields, Stars: Mass Loss, X-Rays: Stars

Scientific paper

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.

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