3-D Simulations of Magnetic Massive Star Winds
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.
- Publication:
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Proceedings of a Scientific Meeting in Honor of Anthony F. J. Moffat
- Pub Date:
- December 2012
- DOI:
- 10.48550/arXiv.1203.1523
- arXiv:
- arXiv:1203.1523
- Bibcode:
- 2012ASPC..465...60U
- Keywords:
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- Astrophysics - Solar and Stellar Astrophysics
- E-Print:
- 5 pages, Conference Proceedings from Four Decades of Research on Massive Stars: A Scientific Meeting in Honour of Anthony F. J. Moffat