Magnetically driven jets from accretion disks: The effect of magneto-rotational instability |
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Institution: | 1. Princeton University, Princeton, New Jersey 08544, United States of America;2. Princeton Plasma Physics Laboratory, Princeton, New Jersey 08543, United States of America;3. Max Planck Institute for Plasma Physics, Boltzmannstr. 2, Garching, 85748 Germany |
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Abstract: | We present the results of 2.5-dimensional MHD simulations for jet formation from accretion disks in a situation such that the magneto-rotational instability is occurring in the disk. When there is no initial perturbation in the disk, the surface layer falls faster than the equatorial part to make a surface avalanche and associated jets. However, if we input an initially large perturbation (> 10% of sound speed) in the disk, the dense region of the disk falls on an orbital time scale to make a more violent accretion and jet. In this case, the accretion rate and mass loss rates are an order of magnitude larger than those in the case without initial perturbation. The speed of the jet is of order the Keplerian velocity of the disk regardless of the instability. |
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