Stellar winds, magnetic fields and disks

Research output: Chapter in Book/Report/Conference proceedingChapter

3 Scopus citations

Abstract

All main sequence stars lose mass via stellar winds. The winds of cool stars like the sun are driven by gas pressure gradient. However, the winds of hot massive stars which tend to be luminous are driven by emitted by the star radiation pressure. Mass loss from such winds are significantly higher. In this article, I describe the nature of such radiatively driven winds and show how they interact with rotation and magnetic fields leading to stellar spindown and large-scale disk-like structures. In particular, I show that the overall degree to which the wind is influenced by the field depends largely on a single, dimensionless, wind magnetic confinement parameter, η*(= B eqR 2M v∞ , which characterizes the ratio between magnetic field energy density and kinetic energy density of the wind.

Original languageEnglish (US)
Title of host publicationThe Environments of the Sun and the Stars
EditorsJean-Pierre Rozelot, Coralie Neiner
Pages207-230
Number of pages24
DOIs
StatePublished - Jan 1 2013

Publication series

NameLecture Notes in Physics
Volume857
ISSN (Print)0075-8450

All Science Journal Classification (ASJC) codes

  • Physics and Astronomy (miscellaneous)

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    Ud-Doula, A. (2013). Stellar winds, magnetic fields and disks. In J-P. Rozelot, & C. Neiner (Eds.), The Environments of the Sun and the Stars (pp. 207-230). (Lecture Notes in Physics; Vol. 857). https://doi.org/10.1007/978-3-642-30648-8-8