Magnetic fields influence the dynamics of hot-star winds and create large scale structure. Based on numerical magnetohydrodynamic (MHD) simulations, we model the wind of θ¹ Ori C, and then use the SEI method to compute synthetic line profiles for a range of viewing angles as function of rotational phase. The resulting dynamic spectrum for a moderately strong line shows a distinct modulation, but with a phase that seems at odds with available observations.
Identifer | oai:union.ndltd.org:Potsdam/oai:kobv.de-opus-ubp:1801 |
Date | January 2007 |
Creators | ud-Doula, A. |
Publisher | Universität Potsdam, Extern. Extern |
Source Sets | Potsdam University |
Language | English |
Detected Language | English |
Type | InProceedings |
Format | application/pdf |
Rights | http://opus.kobv.de/ubp/doku/urheberrecht.php |
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