Hostname: page-component-cd9895bd7-jn8rn Total loading time: 0 Render date: 2024-12-12T17:50:40.011Z Has data issue: false hasContentIssue false
  • English
  • Français

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

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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

References

Blandford, R.D. & Payne, D.G., MNRAS 199, 883 (1983).Google Scholar
Cammenzind, M., in Accretion Disks and Magnetic Fields in Astrophysics, ed. Belvedere, G. (Dordrecht, Kluwer 1989), p. 129.Google Scholar
Cao, X. & Spruit, H.C., Astronomy and Astrophysics, 287, 80–86 (1994).Google Scholar
Koide, S., Nishikawa, K.-I., & Mutel, R.L., 1996, ApJ, 463, L71–L74.CrossRefGoogle Scholar
Koide, S. 1996, ApJ, submitted.Google Scholar
Kudoh, T. & Shibata, K., ApJ, 452, L41–L44 (1995).Google Scholar
Li, Z.-Y., Chiueh, T., & Begelman, M.C., ApJ, 394, 459–471 (1992).Google Scholar
Miley, G.K., 1980, A. Rev. Astr. Astrophys. 18, 165.Google Scholar
Mirabel, I.F. & Rodriguez, L.F., Nature, 371, 46–48 (1994).Google Scholar
Mirabel, I.F., & Rodriguez, L.F., Proc. NATO ASI, Solar and Astrophysical MHD Flows, ed. Tsinganos, K.C., (Heraklion, Kluwer 1996), p. 683.Google Scholar
Shibata, K. & Uchida, Y., Publ. Astron. Soc. Japan, 38, 631–660 (1986).Google Scholar
Tomimatsu, A., Publ. Astron. Soc. Japan, 46, 123–130 (1994).Google Scholar