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Title:
Outflows and accretion in a star-disc system with stellar magnetosphere and disc dynamo
Authors:
von Rekowski, B.; Brandenburg, A.
Affiliation:
AA(Department of Astronomy & Space Physics, Uppsala University, Box 515, 751 20 Uppsala, Sweden), AB(NORDITA, Blegdamsvej 17, 2100 Copenhagen Ø, Denmark)
Publication:
Astronomy and Astrophysics, v.420, p.17-32 (2004) (A&A Homepage)
Publication Date:
06/2004
Origin:
A&A
Astronomy Keywords:
ISM: jets and outflows, accretion, accretion disks, magnetic fields, magnetohydrodynamics (MHD)
DOI:
10.1051/0004-6361:20034065
Bibliographic Code:
2004A&A...420...17V

Abstract

The interaction between a protostellar magnetosphere and a surrounding dynamo-active accretion disc is investigated using an axisymmetric mean-field model. In all models investigated, the dynamo-generated magnetic field in the disc arranges itself such that in the corona, the field threading the disc is anti-aligned with the central dipole so that no X-point forms. When the magnetospheric field is strong enough (stellar surface field strength around 2 kG or larger), accretion happens in a recurrent fashion with periods of around 15 to 30 days, which is somewhat longer than the stellar rotation period of around 10 days. In the case of a stellar surface field strength of at least a few 100 G, the star is being spun up by the magnetic torque exerted on the star. The stellar accretion rates are always reduced by the presence of a magnetosphere which tends to divert a much larger fraction of the disc material into the wind. Both, a pressure-driven stellar wind and a disc wind form. In all our models with disc dynamo, the disc wind is structured and driven by magneto-centrifugal as well as pressure forces.
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