A Non-Magnetocentrifugal Jet Model for Young Stellar Objects

Details A Non-Magnetocentrifugal Jet Model for Young Stellar Objects A Non-Magnetocentrifugal Jet Model for Young Stellar Objects

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20921913w&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #219.13; Bulletin of the American Astronomical Society,

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Scientific paper

Many detailed observations of jet launching in young stellar objects (YSOs) appear consistent with magnetocentrifugal models of acceleration. This has been interpreted as support for these models. There are other possibilities, however.
In previous work, I described how turbulence driven by the magnetorotational instability (MRI) may help launch jets. As conceived and formulated, this jet launching mechanism is not magnetocentrifugal. The MRI-driven magnetohydrodynamic (MHD) turbulence creates hoop-stresses both on and above the midplane, and I suggested that these confine and collimate the outflow. This is fundamentally different from far-downstream hoop-stress collimation of jets beyond the Alfvén surface such as occurs in traditional magnetocentrifugal jet mechanisms. Indeed, in standard MHD wind theory, the hoop-stress must vanish on the midplane.
There now exist substantial observational constraints on several quantities fundamental to jet launching in YSOs, including the ratio of jet mass flux to accretion mass flux, the jet thrust, and the jet angular momentum flux. Here I show that this consistency is not as robust a test of magnetocentrifugal acceleration as might be hoped.
In particular, I construct a non-magnetocentrifugal jet model based on MRI-driven turbulent jet confinement and collimation. I show how this model may explain jets in YSOs consistently with the observational constraints, especially in high accretion-rate systems. Finally, I discuss potential observational discriminants between this preliminary model and the magnetocentrifugal class of models.

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