期刊
ASTRONOMISCHE NACHRICHTEN
卷 327, 期 4, 页码 340-354出版社
WILEY-V C H VERLAG GMBH
DOI: 10.1002/asna.200510526
关键词
ISM : jets and outflows; accretion, accretion disks; magnetohydrodynamics (MHD); stars : mass-loss; stars : pre-main sequence
We have carried out global three-dimensional magnetohydrodynamic simulations of the star-disc interaction region around a young solar-type star. T'he magnetic field is generated and maintained by dynamos in the star as well as in the disc. The developing mass flows possess non-periodic time-variable azimuthal structure and are controlled by the nonaxisymmetric magnetic fields. Since the stellar field drives a strong stellar wind, accretion is anti-correlated with the stellar field strength and disc matter is spiraling onto the star at low latitudes, both contrary to the generally assumed accretion picture. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.
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