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Título

Microscopic Processes in Global Relativistic Jets Containing Helical Magnetic Fields

AutorNishikawa, Ken-Ichi; Mizuno, Yosuke; Niemiec, Jacek; Kobzar, Oleh; Pohl, Martin; Gómez Fernández, J. L. ; Duţan, Ioana; Pe’er, Asaf; Frederiksen, Jacob Trier; Nordlund, Åke; Meli, Athina; Sol, Helene; Hardee, Philip E.; Hartmann, Dieter H.
Fecha de publicación29-sep-2016
EditorMultidisciplinary Digital Publishing Institute
CitaciónGalaxies 4(4): 38 (2016)
ResumenIn the study of relativistic jets one of the key open questions is their interaction with the environment on the microscopic level. Here, we study the initial evolution of both electron–proton (<inline-formula> <math display="inline"> <semantics> <msup> <mi>e</mi> <mo>−</mo> </msup> </semantics> </math> </inline-formula>–<inline-formula> <math display="inline"> <semantics> <msup> <mi>p</mi> <mo>+</mo> </msup> </semantics> </math> </inline-formula>) and electron–positron (<inline-formula> <math display="inline"> <semantics> <msup> <mi>e</mi> <mo>±</mo> </msup> </semantics> </math> </inline-formula>) relativistic jets containing helical magnetic fields, focusing on their interaction with an ambient plasma. We have performed simulations of “global” jets containing helical magnetic fields in order to examine how helical magnetic fields affect kinetic instabilities such as the Weibel instability, the kinetic Kelvin-Helmholtz instability (kKHI) and the Mushroom instability (MI). In our initial simulation study these kinetic instabilities are suppressed and new types of instabilities can grow. In the <inline-formula> <math display="inline"> <semantics> <msup> <mi>e</mi> <mo>−</mo> </msup> </semantics> </math> </inline-formula>–<inline-formula> <math display="inline"> <semantics> <msup> <mi>p</mi> <mo>+</mo> </msup> </semantics> </math> </inline-formula> jet simulation a recollimation-like instability occurs and jet electrons are strongly perturbed. In the <inline-formula> <math display="inline"> <semantics> <msup> <mi>e</mi> <mo>±</mo> </msup> </semantics> </math> </inline-formula> jet simulation a recollimation-like instability occurs at early times followed by a kinetic instability and the general structure is similar to a simulation without helical magnetic field. Simulations using much larger systems are required in order to thoroughly follow the evolution of global jets containing helical magnetic fields.
URIhttp://hdl.handle.net/10261/142114
DOIhttp://dx.doi.org/10.3390/galaxies4040038
Identificadoresdoi: 10.3390/galaxies4040038
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