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General Relativistic Simulation of Jet Formation from Magnetized Accretion Disk

Published online by Cambridge University Press:  12 April 2016

Shinji Koide ,
Kazunari Shibata  and
Takahiro Kudoh
Shinji Koide
Affiliation:
Faculty of Engineering, Toyama University, Gofuku, Toyama 930, Japan
Kazunari Shibata
Affiliation:
National Astromonical Observatory, Mitaka, Tokyo 181, Japan
Takahiro Kudoh
Affiliation:
National Astromonical Observatory, Mitaka, Tokyo 181, Japan

Abstract

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Recently, superluminal motions are observed not only from active galactic nuclei but also in our Galaxy. These phenomena are explained as relativistic jets propagating almost toward us with Lorentz factor more than 2. For the formation of such a relativistic jet, magnetically driven mechanism around a black hole is most promising. We have extended the 2.5D Newtonian MHD jet model (Shibata & Uchida 1986) to general relativistic regime. For this purpose, we have developed a general relativistic magnetohydrodynamic (GRMHD) numerical code and applied it to the simulation of the magnetized accretion disk around a black hole. We have found the formation of magnetically driven jets with 86 percent of light velocity (i.e. Lorentz factor ~ 2.0).

Type
Part 14. AGN and Galactic Centre
Information
International Astronomical Union Colloquium , Volume 163: Accretion Phenomena and Related Outflows , 1997 , pp. 667 - 671
Copyright
Copyright © Astronomical Society of the Pacific 1997

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