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RESEARCH PRODUCT
Recollimation shocks in relativistic jets
Jose Manuel MartíManel PeruchoAntonio FuentesJosé L. Gómezsubject
Shock waveactive [Galaxies]Radio galaxyAstrophysics::High Energy Astrophysical PhenomenaContext (language use)Astrophysics01 natural sciencesShock wavesMagnetohydrodynamicsAstrophysical jet0103 physical sciencesRadiation mechanisms: nonthermal010303 astronomy & astrophysicsAstrophysics::Galaxy AstrophysicsMathematical PhysicsPhysicsnumerical [Methods]Methods: numericalComputer simulation010308 nuclear & particles physicsAstronomy and AstrophysicsQuasarGalaxies: activenonthermal [Radiation mechanisms]Magnetic fieldGalaxies: jetsSpace and Planetary Sciencejets [Galaxies]Magnetohydrodynamicsdescription
Recollimation shocks (RS) appear associated with relativistic flows propagating through pressure mismatched atmospheres. Astrophysical scenarios invoking the presence of such shocks include jets from AGNs and X-ray binaries and GRBs. We shall start reviewing the theoretical background behind the structure of RS in overpressured jets. Next, basing on numerical simulations, we will focus on the properties of RS in relativistic steady jets threaded by helical magnetic fields depending on the dominant type of energy. Synthetic radio maps from the simulation of the synchrotron emission for a selection of models in the context of parsec-scale extragalactic jets will also be discussed.© 2018 World Scientific Publishing Company.
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2018-07-01 | International Journal of Modern Physics D |