Large-scale wind structure due to magnetic fields

  • 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.

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Metadaten
Author details:A. ud-Doula
URN:urn:nbn:de:kobv:517-opus-18010
Publication type:Conference Proceeding
Language:English
Publication year:2007
Publishing institution:Universität Potsdam
Release date:2008/04/25
RVK - Regensburg classification:US 1999.07
Organizational units:Extern / Extern
DDC classification:5 Naturwissenschaften und Mathematik / 52 Astronomie / 520 Astronomie und zugeordnete Wissenschaften
Collection(s):Universität Potsdam / Tagungsbände/Proceedings (nicht fortlaufend) / Clumping in hot-star winds: International Workshop, Potsdam, Germany, 18. - 22. June 2007
Universität Potsdam / Tagungsbände/Proceedings (nicht fortlaufend) / Clumping in hot-star winds: International Workshop, Potsdam, Germany, 18. - 22. June 2007 / Talks and Discussions (in alphabetical order)
Universität Potsdam / Tagungsbände/Proceedings (nicht fortlaufend) / Clumping in hot-star winds: International Workshop, Potsdam, Germany, 18. - 22. June 2007 / Talks and Discussions (organized by sections) / Hydrodynamic modeling (stationary)
License (German):License LogoKeine öffentliche Lizenz: Unter Urheberrechtsschutz
External remark:
The complete edition of the proceedings "Clumping in hot-star winds" is available:
urn:nbn:de:kobv:517-opus-13981
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