Time-dependent simulations of high energy emission of Blazars by a relativistic electron-positron jet

We present first results from a numerical code developed to study the time-dependent simulations of the high energy emission of a relativistic electron-positron jet. High energy emission is due to Inverse Compton radiation on to soft photons coming from a standard accretion disk arround a supermassive black hole. The pair plasma is accelerated by the turbulence triggered by a surrounding jet ('two-flow' model). When particles are accelerated above the pair creation threshold a dense pair plasma can develop drawing energy from the turbulence. When the pair energy density is above the local magnetic density the acceleration mechanism becomes inefficient and the pair creation stops. This model can account for the ejection of pair plasma and for the variability in the high energy emission of Blazars on time scale as short as a few r_g/c (where r_g is the Schwarzschild radius of the black hole).