Magnetohydrodynamic Simulation of Jet Formation in Close Vicinity of Rotating Black Hole

Details Magnetohydrodynamic Simulation of Jet Formation in Close Vicinity of Rotating Black Hole Magnetohydrodynamic Simulation of Jet Formation in Close Vicinity of Rotating Black Hole

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998tx19.confe.413k&link_type=abstract

Abstracts of the 19th Texas Symposium on Relativistic Astrophysics and Cosmology, held in Paris, France, Dec. 14-18, 1998. Eds.:

Astronomy and Astrophysics

Astrophysics

Scientific paper

Astrophysical jets from AGNs and microquasars are separated into two classes; relativistic (Lorentz factor ~2-20) and sub-relativistic one (velocity ~0.1-0.3c). It is believed that the jets of both classes are formed near the central highly condensed objects: black holes or neutron stars. Some observations suggest that the rotation of the central objects determine the speed of the jets. In fact, general relativistic MHD simulations of Schwarzshild black hole magnetosphere with falling corona never show the highly relativistic jets (Koide, Shibata, & Kudoh 1998). The fast rotating black hole is expected to form the highly relativistic jets. In this paper, we report a first numerical simulations of relativistic jet formation in the Kerr black hole magnetosphere.

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