Shock Acceleration at Super-luminal Relativistic Shocks - A Numerical Study

Details Shock Acceleration at Super-luminal Relativistic Shocks - A Numerical Study Shock Acceleration at Super-luminal Relativistic Shocks - A Numerical Study

Oct 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004vhec.conf..169m&link_type=abstract

Presented at XIII International Symposium of Very High Energy Cosmic Ray Interactions, Pylos, Greece; September 2004, p. 29-33

Astronomy and Astrophysics

Astrophysics

Cosmic Rays, Super-Luminal Shocks, Acceleration

Scientific paper

We present Monte Carlo calculations of the Cosmic Ray spectral shapes and Cosmic Ray energy gains for diffusive shock acceleration at super-luminal shock waves, with high upstream flow Lorentz gamma factors, from 10 up to 500, which could be relevant to models of relativistic astrophysical environments like AGN jets and GRB sites. Both large angle and pitch angle diffusion of the accelerated Cosmic Rays is considered, applying to the relevant astrophysical models. Our physical/numerical approach allows that the particle's trajectory is followed along the magnetic field lines during shock crossings where the equivalent of a guiding centre approximation is inappropriate, constantly measuring its phase space co-ordinates in the fluid frames, where E=0. We find striking differences in the Cosmic Ray energy spectra while using large angle scattering versus pitch angle diffusion methods; showing that the Cosmic Ray pitch angle diffusion in highly relativistic super-luminal shocks, could be the 'key' for the Very High Energy Cosmic Ray (VHECR) to be produced in plausible astrophysical sites as AGN jets and GRBs.

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