Dynamos in accretion discs

Details Dynamos in accretion discs Dynamos in accretion discs

2007-02-19

arxiv.org/abs/astro-ph/0702493v1

Mem.Soc.Ast.It.78:374-381,2007

Astronomy and Astrophysics

Astrophysics

8 pages, 7 figures, proceedings of Coronae of Stars and Accretion Disks, Bonn, December 2006, to be published in Memorie della

Scientific paper

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.

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