Magnetically confined wind shocks in X-rays - A review

ud-Doula, Asif; Nazé, Yaël

doi:10.1016/j.asr.2015.09.025

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Magnetically confined wind shocks in X-rays - A review

ud-Doula, Asif; Nazé, Yaël

2016 • In Advances in Space Research, 58, p. 680-693

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https://hdl.handle.net/2268/202265

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10.1016/j.asr.2015.09.025

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Keywords :

X-rays; MHD; Massive stars

Abstract :

[en] A subset (∼ 10%) of massive stars present strong, globally ordered (mostly dipolar) magnetic fields. The trapping and channeling of their stellar winds in closed magnetic loops leads to magnetically confined wind shocks (MCWS), with pre-shock flow speeds that are some fraction of the wind terminal speed. These shocks generate hot plasma, a source of X-rays. In the last decade, several developments took place, notably the determination of the hot plasma properties for a large sample of objects using XMM and Chandra, as well as fully self-consistent MHD modeling and the identification of shock retreat effects in weak winds. Despite a few exceptions, the combination of magnetic confinement, shock retreat and rotation effects seems to be able to account for X-ray emission in massive OB stars. Here we review these new observational and theoretical aspects of this X-ray emission and envisage some perspectives for the next generation of X-ray observatories.

Disciplines :

Space science, astronomy & astrophysics

Author, co-author :

ud-Doula, Asif; Penn State Worthington Scranton, 120 Ridge View Drive, Dunmore, PA 18512, USA

Nazé, Yaël ; Université de Liège > Groupe d'astrophysique des hautes énergies (GAPHE)

Language :

English

Title :

Magnetically confined wind shocks in X-rays - A review

Publication date :

01 September 2016

Journal title :

Advances in Space Research

ISSN :

0273-1177

eISSN :

1879-1948

Publisher :

Pergamon Press, Oxford, United Kingdom

Volume :

Pages :

680-693

Peer reviewed :

Peer Reviewed verified by ORBi

Additional URL :

http://cdsads.u-strasbg.fr/abs/2016AdSpR..58..680U

Available on ORBi :

since 03 October 2016

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