2012/03/07 by Asif ud‐Doula, Asif ud-Doula, ud-Doula, Asif
Physics and Astronomy · #Astro and Planetary Science #FOS: Physical sciences #Ionosphere and magnetosphere dynamics #Solar and Space Plasma Dynamics #Solar and Stellar Astrophysics (astro-ph.SR) #astro-ph.SR
paper · pdf · doi:10.48550/arxiv.1203.1523
5 pages, Conference Proceedings from Four Decades of Research on Massive Stars: A Scientific Meeting in Honour of Anthony F. J. Moffat
arxiv created 2012/03/07 · openalex publication_date 2012/03/07 · arxiv updated 2012/03/08 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Due to computational requirements and numerical difficulties associated with coordinate singularity in spherical geometry, fully dynamic 3D magnetohydrodynamic (MHD) simulations of massive star winds are not readily available. Here we report preliminary results of the first such a 3D 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 magnetically confined wind shock (MCWS) is the dominating mechanism for hard Xrays in some massive stars.