Large scale magnetic fields in discs: jets and reconnection X-winds

Details Large scale magnetic fields in discs: jets and reconnection X-winds Large scale magnetic fields in discs: jets and reconnection X-winds

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007iaus..243..307f&link_type=abstract

Star-Disk Interaction in Young Stars, Proceedings of the International Astronomical Union, IAU Symposium, Volume 243, p. 307-314

Other

Accretion Discs, Magnetohydrodynamics, Stars: Pre-Main Sequence, Stars: Magnetic Fields, Stars: Rotation, Ism: Jets And Outflows

Scientific paper

In this contribution we first briefly review our current knowledge on the physics of accretion discs driving self-confined jets. It will be shown that a large scale magnetic field is expected to thread the innermost disc regions, giving rise to a transition from an outer standard accretion disc to an inner jet emitting disc. We then report new progresses on the theory of star-disc interaction, allowing to explain the formation of accretion funnel flows with stellar dipole fields consistent with observational constraints. Such a connection is now not only probed by modern observations but it is also requested for spinning down protostars, which are known to be both actively accreting and contracting. This spin down most probably relies on the angular momentum removal by ejection. Two such scenarios will be addressed here, namely “accretion-powered stellar winds” (Matt & Pudritz 2005) and “Reconnection X-winds” (Ferreira, Pelletier & Appl 2000). The latter can slow down a protostar on time scales shorter or comparable to the embedded phase. It will be shown that these two scenarios are not incompatible and that transitions from one to another may even occur as they mainly depend on the stellar dynamo.

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