Simulation of Relativistic Jets with Macroscopic and Microscopic Processes and Associated Self-consistent Radiation

Relativistic jets are ubiquitous in astrophysical systems. In this talk I will present recent research results from RMHD simulations designed to study the CD kink instability of relativistic jets and the magnetic field amplification that occurs in relativistic shocks in an inhomogeneous medium. I will then present the results of RPIC simulations of particle acceleration in relativistic shocks and self-consistent calculation of the radiation at the microscopic level. In these collisionless relativistic shocks plasma instabilities are responsible for particle acceleration. In particular I will show the particle acceleration and shock structure associated with an unmagnetized relativistic electron-positron jet propagating into an unmagnetized electron-positron plasma, i.e., a hydrodynamic relativistic shock. Strong electromagnetic fields are generated in the trailing shock and provide an emission site. These magnetic fields contribute to the electrons transverse deflection behind the shock. We calculate the radiation from electrons deflected in the turbulent magnetic fields. The properties of this radiation are important for understanding the complex time evolution and spectral structure in gamma-ray burst, relativistic jet, and supernova shocks.


20/06/2011 - 14:00
Ken Nishikawa
Univ. of Alabama, Huntsville/CSPAR, USA