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- W4312693990 abstract "Many stars across all classes possess strong enough magnetic fields to influence dynamical flow of material off the stellar surface. For the case of massive stars (O and B types), about 10% of them harbor 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 that can be a few thousand km s−1. 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-Newton and Chandra, as well as fully self-consistent MHD modeling and the identification of shock retreat effects in weak winds. In addition, these objects are often sources of Hα emission which is controlled by either sufficiently high mass loss rate or centrifugal breakout. Here we review the theoretical aspects of such magnetic massive star wind dynamics." @default.
- W4312693990 created "2023-01-05" @default.
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- W4312693990 date "2022-09-26" @default.
- W4312693990 modified "2023-09-24" @default.
- W4312693990 title "Magnetically Confined Wind Shock" @default.
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- W4312693990 doi "https://doi.org/10.1007/978-981-16-4544-0_80-1" @default.
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