Energy release in strongly magnetized relativistic winds

Details Energy release in strongly magnetized relativistic winds Energy release in strongly magnetized relativistic winds

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992sval...18..356l&link_type=abstract

Soviet Astronomy Letters, Vol. 18, p. 356; Pis'ma v Astronomicheskii Zhurnal (ISSN 0320-0108), vol. 18, no. 10, p. 878-886. In

Astronomy and Astrophysics

Astronomy

11

Active Galactic Nuclei, Magnetohydrodynamic Flow, Magnetohydrodynamic Stability, Pulsars, Relativistic Plasmas, Stellar Magnetic Fields, Accretion Disks, Black Holes (Astronomy), Neutron Stars, Stellar Rotation

Scientific paper

Relativistic winds generated by a strongly magnetized rotating body (a neutron star, an accretion disc, or a black hole) cannot be terminated by a shock wave. Rotation energy which is extracted from the central body by the electromagnetic stresses and stored in the magnetic field is released due to MHD instabilities of relevant magnetic configurations. This scenario is discussed for cases of AGNs and pulsars.

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