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Paper: 3-D Simulations of Magnetic Massive Star Winds
Volume: 465, Four Decades of Massive Star Research - A Scientific Meeting in Honor of Anthony J. Moffat
Page: 60
Authors: ud-Doula, A.
Abstract: Due to computational requirements and numerical difficulties associated with coordinate singularity in spherical geometry, fully dynamic 3-D magnetohydrodynamic (MHD) simulations of massive star winds are not readily available. Here we report preliminary results of the first such a 3-D simulation using θ1 Ori C (O5.5 V) as a model. The oblique magnetic rotator θ1 Ori C is a source of hard X-ray emitting plasma in its circumstellar environment. Our numerical model can explain both the hardness and the location of the X-ray emission from this star confirming that a magnetically confined wind shock (MCWS) is the dominating mechanism for hard X-rays in some massive stars.
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