Document Type

Conference Proceeding

Publication Date

8-1-2013

Published In

Proceedings Of The International Astronomical Union

Abstract

A subpopulation (~10%) of hot, luminous, massive stars have been revealed through spectropolarimetry to harbor strong (hundreds to tens of thousand Gauss), steady, large-scale (often significantly dipolar) magnetic fields. This review focuses on the role of such fields in channeling and trapping the radiatively driven wind of massive stars, including both in the strongly perturbed outflow from open field regions, and the wind-fed “magnetospheres” that develop from closed magnetic loops. For B-type stars with weak winds and moderately fast rotation, one finds “centrifugal magnetospheres”, in which rotational support allows magnetically trapped wind to accumulate to a large density, with quite distinctive observational signatures, e.g. in Balmer line emission. In contrast, more luminous O-type stars have generally been spun down by magnetic braking from angular momentum loss in their much stronger winds. The lack of centrifugal support means their closed loops form a “dynamical magnetosphere”, with trapped material falling back to the star on a dynamical timescale; nonetheless, the much stronger wind feeding leads to a circumstellar density that is still high enough to give substantial Balmer emission. Overall, this review describes MHD simulations and semi-analytic dynamical methods for modeling the magnetospheres, the magnetically channeled wind outflows, and the associated spin-down of these magnetic massive stars.

Keywords

Stars – early-type, Stars – magnetic fields, Stars – mass loss, Stars – X-rays, Stars – Rotation

Conference

Magnetic Fields Throughout Stellar Evolution

Conference Dates

Aug. 25-30, 2013

Conference Location

Biarritz, France

Comments

This work is a preprint that is freely available courtesy of Cambridge University Press and the International Astronomical Union.

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