Dynamos in accretion discs
天体物理学
2011-04-28 v1
摘要
It is argued that accretion discs in young stellar objects may have hot coronae that are heated by magnetic reconnection. This is a consequence of the magneto-rotational instability driving turbulence in the disc. Magnetic reconnection away from the midplane leads to heating of the corona which, in turn, contributes to driving disc winds.
引用
@article{arxiv.astro-ph/0702493,
title = {Dynamos in accretion discs},
author = {A. Brandenburg and B. von Rekowski},
journal= {arXiv preprint arXiv:astro-ph/0702493},
year = {2011}
}
备注
8 pages, 7 figures, proceedings of Coronae of Stars and Accretion Disks, Bonn, December 2006, to be published in Memorie della Societa Astronomica Italiana