2024-03-29T01:11:17Zhttp://digital.csic.es/dspace-oai/requestoai:digital.csic.es:10261/1421222018-08-02T11:14:17Zcom_10261_97com_10261_4col_10261_350
00925njm 22002777a 4500
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Mizuno, Yosuke
author
Gómez Fernández, J. L.
author
Nishikawa, Ken-Ichi
author
Meli, Athina
author
Hardee, Philip E.
author
Rezzolla, Luciano
author
Singh, Chandra B.
author
Pino, Elisabete M. de Gouveia Dal
author
2016-10-07
The most promising mechanisms for producing and accelerating relativistic jets, and maintaining collimated structure of relativistic jets involve magnetohydrodynamical (MHD) processes. We have investigated the magnetic dissipation mechanism in relativistic jets via relativistic MHD simulations. We found that the relativistic jets involving a helical magnetic field are unstable for the current-driven kink instability, which leads to helically distorted structure in relativistic jets. We identified the regions of high current density in filamentary current sheets, indicative of magnetic reconnection, which are associated to the kink unstable regions and correlated to the converted regions of magnetic to kinetic energies of the jets. We also found that an over-pressured relativistic jet leads to the generation of a series of stationary recollimation shocks and rarefaction structures by the nonlinear interaction of shocks and rarefaction waves. The differences in the recollimation shock structure due to the difference of the magnetic field topologies and strengths may be observable through mm-VLBI observations and space-VLBI mission.
Galaxies 4(4): 40 (2016)
http://hdl.handle.net/10261/142122
10.3390/galaxies4040040
http://dx.doi.org/10.13039/501100003339
http://dx.doi.org/10.13039/501100003329
http://dx.doi.org/10.13039/501100000781
Magnetic Dissipation in Relativistic Jets