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General-Relativistic MHD Simulation of Jets from a Geometrically Thin Accretion Disk Around a Schwarzschild Black Hole

Published online by Cambridge University Press:  25 May 2016

S. I. Aoki ,
S. Koide ,
K. Shibata  and
T. Kudoh
S. I. Aoki
Affiliation:
Department of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan
S. Koide
Affiliation:
Faculty of Engineering, Toyama University, Gofuku, Toyama 930, Japan
K. Shibata
Affiliation:
Kwasan and Hida Observatories, Kyoto University, Yamashina, Kyoto 607-8471, Japan
T. Kudoh
Affiliation:
Solar Physics Division, National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan

Abstract

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We have performed a 2.5D, nonsteady, general-relativistic MHD simulation. Initially, we assumed a uniform magnetic field, a geometrically thin accretion disk rotating at Keplerian velocity, and a hydrostatic corona around a Schwarzschild black hole. We have investigated the formation mechanism of gas-pressure driven jets expected by Koide et al. and found the strong dependence of jet velocities Lorentz factor of jets) on the ratio of the density of the accretion disk to that of the corona (ρd/ρc), where γ2j - γj ∝ (ρd/ρc)0.75.

Type
Part II: Posters
Information
Symposium - International Astronomical Union , Volume 195: Highly Energetic Physical Processes and Mechanisms , 2000 , pp. 373 - 374
Copyright
Copyright © Astronomical Society of the Pacific 2000 

References

Koide, S., Shibata, K., & Kudoh, T. 1998, ApJ, 495, L63.Google Scholar
Shibata, K., & Uchida, Y. 1986, PASJ, 38, 631.Google Scholar
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