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Recollimation shocks in magnetized relativistic jets

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Abstract
We have performed two-dimensional special-relativistic magnetohydrodynamic simulations of non-equilibrium over-pressured relativistic jets in cylindrical geometry. Multiple stationary recollimation shock and rarefaction structures are produced along the jet by the nonlinear interaction of shocks and rarefaction waves excited at the interface between the jet and the surrounding ambient medium. Although initially the jet is kinematically dominated, we have considered axial, toroidal, and helical magnetic fields to investigate the effects of different magnetic-field topologies and strengths on the recollimation structures. We find that an axial field introduces a larger effective gas pressure and leads to stronger recollimation shocks and rarefactions, resulting in larger flow variations. The jet boost grows quadratically with the initial magnetic field. On the other hand, a toroidal field leads to weaker recollimation shocks and rarefactions, significantly. modifying the jet structure after the first recollimation rarefaction and shock. The jet boost decreases systematically. For a helical field, instead, the behavior depends on the magnetic pitch, with a phenomenology that ranges between the one seen for axial and toroidal magnetic fields, respectively. In general, however, a helical magnetic field yields a more complex shock and rarefaction substructure close to the inlet that significantly modifies the jet structure. The differences in shock structure resulting from different field configurations and strengths may have observable consequences for disturbances propagating through a stationary recollimation shock.
Keywords
magnetohydrodynamics (MHD), galaxies: jets, methods: numerical, shock waves, CURRENT-DRIVEN INSTABILITY, ACTIVE GALACTIC NUCLEUS, MAGNETOHYDRODYNAMIC SIMULATIONS, M87 JET, NUMERICAL SIMULATIONS, SYNCHROTRON EMISSION, SUPERLUMINAL SOURCES, RADIO-SOURCES, INNER JET, ACCELERATION

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MLA
Mizuno, Yosuke et al. “Recollimation Shocks in Magnetized Relativistic Jets.” ASTROPHYSICAL JOURNAL 809.1 (2015): n. pag. Print.
APA
Mizuno, Y., Gómez, J. L., Nishikawa, K.-I., Meli, A., Hardee, P. E., & Rezzolla, L. (2015). Recollimation shocks in magnetized relativistic jets. ASTROPHYSICAL JOURNAL, 809(1).
Chicago author-date
Mizuno, Yosuke, Jose L Gómez, Ken-Ichi Nishikawa, Athina Meli, Philip E Hardee, and Luciano Rezzolla. 2015. “Recollimation Shocks in Magnetized Relativistic Jets.” Astrophysical Journal 809 (1).
Chicago author-date (all authors)
Mizuno, Yosuke, Jose L Gómez, Ken-Ichi Nishikawa, Athina Meli, Philip E Hardee, and Luciano Rezzolla. 2015. “Recollimation Shocks in Magnetized Relativistic Jets.” Astrophysical Journal 809 (1).
Vancouver
1.
Mizuno Y, Gómez JL, Nishikawa K-I, Meli A, Hardee PE, Rezzolla L. Recollimation shocks in magnetized relativistic jets. ASTROPHYSICAL JOURNAL. 2015;809(1).
IEEE
[1]
Y. Mizuno, J. L. Gómez, K.-I. Nishikawa, A. Meli, P. E. Hardee, and L. Rezzolla, “Recollimation shocks in magnetized relativistic jets,” ASTROPHYSICAL JOURNAL, vol. 809, no. 1, 2015.
@article{7278166,
  abstract     = {We have performed two-dimensional special-relativistic magnetohydrodynamic simulations of non-equilibrium over-pressured relativistic jets in cylindrical geometry. Multiple stationary recollimation shock and rarefaction structures are produced along the jet by the nonlinear interaction of shocks and rarefaction waves excited at the interface between the jet and the surrounding ambient medium. Although initially the jet is kinematically dominated, we have considered axial, toroidal, and helical magnetic fields to investigate the effects of different magnetic-field topologies and strengths on the recollimation structures. We find that an axial field introduces a larger effective gas pressure and leads to stronger recollimation shocks and rarefactions, resulting in larger flow variations. The jet boost grows quadratically with the initial magnetic field. On the other hand, a toroidal field leads to weaker recollimation shocks and rarefactions, significantly. modifying the jet structure after the first recollimation rarefaction and shock. The jet boost decreases systematically. For a helical field, instead, the behavior depends on the magnetic pitch, with a phenomenology that ranges between the one seen for axial and toroidal magnetic fields, respectively. In general, however, a helical magnetic field yields a more complex shock and rarefaction substructure close to the inlet that significantly modifies the jet structure. The differences in shock structure resulting from different field configurations and strengths may have observable consequences for disturbances propagating through a stationary recollimation shock.},
  articleno    = {38},
  author       = {Mizuno, Yosuke and Gómez, Jose L and Nishikawa, Ken-Ichi and Meli, Athina and Hardee, Philip E and Rezzolla, Luciano},
  issn         = {0004-637X},
  journal      = {ASTROPHYSICAL JOURNAL},
  keywords     = {magnetohydrodynamics (MHD),galaxies: jets,methods: numerical,shock waves,CURRENT-DRIVEN INSTABILITY,ACTIVE GALACTIC NUCLEUS,MAGNETOHYDRODYNAMIC SIMULATIONS,M87 JET,NUMERICAL SIMULATIONS,SYNCHROTRON EMISSION,SUPERLUMINAL SOURCES,RADIO-SOURCES,INNER JET,ACCELERATION},
  language     = {eng},
  number       = {1},
  pages        = {14},
  title        = {Recollimation shocks in magnetized relativistic jets},
  url          = {http://dx.doi.org/10.1088/0004-637X/809/1/38},
  volume       = {809},
  year         = {2015},
}

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