Radiation from accelerated particles in relativistic jets with shocks, shear-flow, and reconnection

Abstract

We have investigated particle acceleration and shock structure associated with an unmagnetized relativistic jet propagating into an unmagnetized plasma. Strong magnetic fields generated in the trailing jet shock lead to transverse deflection and acceleration of the electrons. We have self-consistently calculated the radiation from the electrons accelerated in the turbulent magnetic fields. We find that the synthetic spectra depend on the bulk Lorentz factor of the jet, the jet temperature, and the strength of the magnetic fields generated in the shock. We have also begun study of electron acceleration in the strong magnetic fields generated by kinetic shear (Kelvin-Helmholtz) instabilities. Our calculated spectra should lead to a better understanding of the complex time evolution and/or spectral structure from gamma-ray bursts, relativistic jets, and supernova remnants.

6 pages, 4 figures, 2012 Fermi Symposium proceedings - eConf C121028

References in corpus (6)

• Fast TeV variability in blazars: jets in a jet
• 3D Relativistic Magnetohydrodynamic Simulations of Magnetized Spine-Sheath Relativistic Jets
• Weibel instability and associated strong fields in a fully 3D simulation of a relativistic shock
• Large-scale magnetic field generation via the kinetic Kelvin-Helmholtz instability in unmagnetized scenarios
• Magnetic Field Generation and Particle Energization at Relativistic Shear Boundaries in Collisionless Electron-Positron Plasmas
• GRB: magnetic fields, cosmic rays, and emission from first principles?

Cited by in corpus (3)

• New constraints on the structure and dynamics of black hole jets
• Magnetic field generation in a jet-sheath plasma via the kinetic Kelvin-Helmholtz instability
• Quantitatively consistent computation of coherent and incoherent radiation in particle-in-cell codes - a general form factor formalism for macro-particles