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New Insights into the Puzzling P-Cygni Profiles of Magnetic Massive Stars

Published online by Cambridge University Press:  28 July 2017

Christiana Erba ,
Alexandre David-Uraz ,
Véronique Petit  and
Stanley P. Owocki
Christiana Erba
Affiliation:
Deptartment of Physics and Astronomy, Bartol Research Institute, University of Delaware, Newark, DE, 19716, USA
Alexandre David-Uraz
Affiliation:
Deptartment of Physics and Astronomy, Bartol Research Institute, University of Delaware, Newark, DE, 19716, USA Department of Physics and Space Sciences, Florida Institute of Technology, Melbourne, FL 32904, USA
Véronique Petit
Affiliation:
Deptartment of Physics and Astronomy, Bartol Research Institute, University of Delaware, Newark, DE, 19716, USA Department of Physics and Space Sciences, Florida Institute of Technology, Melbourne, FL 32904, USA
Stanley P. Owocki
Affiliation:
Deptartment of Physics and Astronomy, Bartol Research Institute, University of Delaware, Newark, DE, 19716, USA
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Abstract

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Magnetic massive stars comprise approximately 10% of the total OB star population. Modern spectropolarimetry shows these stars host strong, stable, large-scale, often nearly dipolar surface magnetic fields of 1 kG or more. These global magnetic fields trap and deflect outflowing stellar wind material, forming an anisotropic magnetosphere that can be probed with wind-sensitive UV resonance lines. Recent HST UV spectra of NGC 1624-2, the most magnetic O star observed to date, show atypically unsaturated P-Cygni profiles in the Civ resonant doublet, as well as a distinct variation with rotational phase. We examine the effect of non-radial, magnetically-channeled wind outflow on P-Cygni line formation, using a Sobolev Exact Integration (SEI) approach for direct comparison with HST UV spectra of NGC 1624-2. We demonstrate that the addition of a magnetic field desaturates the absorption trough of the P-Cygni profiles, but further efforts are needed to fully account for the observed line profile variation. Our study thus provides a first step toward a broader understanding of how strong magnetic fields affect mass loss diagnostics from UV lines.

Keywords

stars: magnetic fieldsstars: mass lossultraviolet: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S329: The Lives and Death-Throes of Massive Stars , November 2016 , pp. 246 - 249
Copyright
Copyright © International Astronomical Union 2017 

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