Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...19915605m&link_type=abstract
American Astronomical Society, 199th AAS Meeting, #156.05; Bulletin of the American Astronomical Society, Vol. 34, p.563
Astronomy and Astrophysics
Astronomy
Scientific paper
Goodson, Winglee, and Böhm recently proposed a time-dependent accretion/ejection mechanism that explains many observational properties of YSO outflows. They showed that the self-consistent interaction between the stellar dipole magnetic field and a differentially rotating accretion disk leads to a cyclical process. During this process, the location of the disk inner edge and the magnetic field topology alternates between a configuration which is ideal for magnetocentrifugal launching of plasma and a configuration which is ideal for field-aligned accretion. Each oscillation results in the launching of a knot of material along the rotation axis. This may provide a natural explaination for knots observed in YSO jets (e.g., HH 30), but there appears to be a discrepancy between the observed and predicted knot spacing. The large number of parameters and the system's complicated behavior make detailed analytical predictions difficult. For this reason, and in order to better understand the disk oscillation process, we have carried out several time-dependent numerical MHD simulations, exploring a range of parameters. In all cases, the disk-magnetosphere interaction results in the same qualitative mechanism, and we confirm that the oscillation period is set by the spin-down time of the disk inner edge. We present the results of these simulations and compare them to a semi-analytical formulation that we develop for the spin-down time. This research was supported by NSF grant AST 97-29096.
Bohm Karl-Heinz
Goodson Anthony Price
Matt Sean
Winglee Robert M.
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