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Numerical Simulation of Relativistic Jet Formation in Black Hole Magnetosphere

Published online by Cambridge University Press:  25 May 2016

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

Extract

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The radio jets ejected from active galactic nuclei (AGNs) sometimes show proper motions with apparent velocity exceeding the speed of light. This phenomenon, called superluminal motion, is explained as relativistic jets propagating in a direction almost toward us, and has been thought to be ejected from the close vicinity of hypothetical supermassive black holes powering AGNs (Rees 1996). The magnetic mechanism has been proposed not only for AGN jets (Lovelace 1976; Blandford & Payne 1983) but also for protostellar jets (Pudritz & Norman 1986; Uchida & Shibata 1985; Shibata & Uchida 1986), although no one has yet performed nonsteady general relativistic magnetohydrodynamic (GRMHD) numerical simulations on the formation of jets from the accretion disk around a black hole.

Type
Session 3: Diagnostics of High Gravity Objects with X- and Gamma Rays
Information
Symposium - International Astronomical Union , Volume 188: The Hot Universe , 1998 , pp. 415 - 416
Copyright
Copyright © Kluwer 1998