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Scientific paper
Dec 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..282k&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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1
Scientific paper
We performed 2.5 dimensional nonsteady MHD numerical simulations of jets from geometrically thin disks including the dynamics of accretion disks self-consistently. For the initial rotational velocity of the disk, we consider two cases, Keplerian cases and sub-Keplerian cases. In Keplerian cases, we found the following results: (1) The ejection point of jets is determined by the effective potential made by the gravitational and centrifugal forces along the magnetic field (Blandford and Payne 1982). (2) The initial acceleration forces of jets is magnetic pressure when the initial magnetic field strength(B0) is weak, and magneto-centrifugal force is effective when B0 is strong. (3) The dependences of the velocity (Vjet) and the mass outflow rate (dot{M}w) on B0 are dot{M}w propto Emg1/2 and Vjet propto left( frac{ΩF2 Emg}{dot{M}w} right)1/3, therefore Vjet propto Emg1/6 where ΩF is the angular velocity of a field line (essentially the Keplerian angular velocity where the jet is ejected), Emg= (magnetic energy/gravitational energy) propto B02. In sub-Keplerian cases, Vjet propto Emg1/6 is satisfied but the other dependences are not always equal to those of Keplerian cases.
Kato Seiichi X.
Kudoh Takahiro
Shibata Kazunari
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