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Title:
Dynamos in accretion discs
Authors:
Brandenburg, A.; von Rekowski, B.
Affiliation:
AA(NORDITA, AlbaNova University Center, SE-10691 Stockholm, Sweden ), AB(School of Mathematics and Statistics, University of St. Andrews, North Haugh, St. Andrews, Fife KY16 9SS, UK)
Publication:
Memorie della Società Astronomica Italiana, v.78, p.374 (2007)
Publication Date:
00/2007
Origin:
MmSAI
Keywords:
ISM: jets and outflows, accretion, accretion discs, magnetohydrodynamics (MHD), stars: mass-loss, stars: pre-main sequence
Bibliographic Code:
2007MmSAI..78..374B

Abstract

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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