Magnetically Driven Outflows from Accretion Disks

Details Magnetically Driven Outflows from Accretion Disks Magnetically Driven Outflows from Accretion Disks

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..286k&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

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This is the first magnetohydrodynamic (MHD) numerical simulation including accretion of a disk, ejection of a jet, acceleration and collimation of the jet, and formation of a bow shock. We extend the the computational region to about 100 times larger than the radius of central star to investigate the collimation of jet and a formation of a bow shock. (It is about 10 times larger than those of the previous works.) We found that both the magnetic field lines and stream lines are collimated by the pinch effect of the toroidal component of the magnetic field that is generated by the differential rotation in the disk. Finally, the bow shock is formed at the head of the jet by the 'piston effect' of the toroidal component of the magnetic field. The result of the large scale simulation should be compared to the high resolution observation by VLBI.

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