Magnetohydrodynamic Effects in Propagating Relativistic Jets: Reverse Shock and Magnetic Acceleration

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dc.creatorMizuno, Yosuke
dc.creatorZhang, Bing
dc.creatorGiacomazzo, Bruno
dc.creatorNishikawa, Ken-Ichi
dc.creatorHardee, Philip E.
dc.creatorNagataki, Shigehiro
dc.creatorHartmann, Dieter H.
dc.date2008-10-15
dc.date2008-11-13
dc.date.accessioned2026-07-07T12:15:51Z
dc.date.available2026-07-07T12:15:51Z
dc.descriptionWe solve the Riemann problem for the deceleration of an arbitrarily magnetized relativistic flow injected into a static unmagnetized medium in one dimension. We find that for the same initial Lorentz factor, the reverse shock becomes progressively weaker with increasing magnetization σ(the Poynting-to kinetic energy flux ratio), and the shock becomes a rarefaction wave when σexceeds a critical value, σ_c, defined by the balance between the magnetic pressure in the flow and the thermal pressure in the forward shock. In the rarefaction wave regime, we find that the rarefied region is accelerated to a Lorentz factor that is significantly larger than the initial value. This acceleration mechanism is due to the strong magnetic pressure in the flow. We discuss the implications of these results for models of gamma-ray bursts and active galactic nuclei.
dc.description13 pages, 3 figures, Accepted to publication in ApJ Letters
dc.identifierhttps://arxiv.org/abs/0810.2779
dc.identifierhttp://arxiv.org/abs/0810.2779
dc.identifierAstrophys.J.Lett.690:L47-L51,2009
dc.identifierdoi:10.1088/0004-637X/690/1/L47
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/211616
dc.subjectAstrophysics
dc.subjectGeneral Relativity and Quantum Cosmology
dc.titleMagnetohydrodynamic Effects in Propagating Relativistic Jets: Reverse Shock and Magnetic Acceleration
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