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First empirical constraints on the low Hα mass-loss rates of magnetic O-stars

Published online by Cambridge University Press:  30 December 2019

Florian A. Driessen ,
Jon O. Sundqvist  and
Gregg A. Wade
Florian A. Driessen
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D box 2401, BE-3001, Leuven, Belgium email: florian.driessen@kuleuven.be
Jon O. Sundqvist
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D box 2401, BE-3001, Leuven, Belgium email: florian.driessen@kuleuven.be
Gregg A. Wade
Affiliation:
Dept. of Physics & Space Science, Royal Military College of Canada, PO Box 17000, Station Forces, Kingston, Ontario, Canada
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Abstract

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A small subset of Galactic O-stars possess surface magnetic fields that alter the outflowing stellar wind by magnetically confining it. Key to the magnetic confinement is that it induces rotational modulation of spectral lines over the full EM domain; this allows us to infer basic quantities, e.g., mass-loss rate and magnetic geometry. Here, we present an empirical study of the Hα line in Galactic magnetic O-stars to constrain the mass fed from the stellar base into the magnetosphere, using realistic multi-dimensional magnetized wind models, and compare with theoretical predictions. Our results suggest that it may be reasonable to use mass-feeding rates from non-magnetic wind theory if the absolute mass-loss rate is scaled down according to the amount of wind material falling back upon the stellar surface. This provides then some empirical support to the proposal that such magnetic O-stars might evolve into heavy stellar-mass black holes (Petit et al.2017).

Keywords

stars: massivestars: magnetic fieldstars: mass-lossstars: windsoutflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 45 - 48
Copyright
© International Astronomical Union 2019 

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