| Type |
Conference Paper |
| Names |
Richard H. D. Townsend |
| Conference Name |
IAU Symposium |
| Volume |
272 |
| Pages |
148-159 |
| Date |
July 1, 2011 |
| URL |
http://adsabs.harvard.edu/abs/2011IAUS..272..148T |
| Library Catalog |
NASA ADS |
| Abstract |
After briefly reviewing the theory behind the radiative line-driven winds of OB stars, I examine the processes that can generate structure in them; these include both intrinsic instabilities, and surface perturbations such as pulsation and rotation. I then delve into wind channeling and confinement by magnetic fields as a mechanism for forming longer-lived circumstellar structures. With a narrative that largely follows the historical progression of the field, I introduce the key insights and results that link the first detection of a magnetosphere, over three decades ago, to the recent direct measurement of magnetic braking in a number of active OB stars. |
| Tags |
Magnetohydrodynamics: MHD, Stars: Mass Loss, outflows, stars: early-type, stars: emission-line, stars: magnetic fields, stars: rotation, stars: winds |