|Abstract : ||AGN Jets are observed to possess various sites of particle acceleration, which gives rise to the observed non-thermal spectra. Diffusive shock acceleration (DSA) and stochastic turbulent acceleration (SA) are the candidates for producing very high energetic particles in weakly magnetized regions. While DSA is a systematic acceleration process, SA is a random energization process, usually modelled as a biased random walk in energy space with a Fokker-Planck equation. Due to the ubiquitous nature of plasma fluctuations, SA gives rise to diffuse emission, whereas DSA leads to localized emission. In astrophysical systems, different acceleration processes work in an integrated manner along with various energy losses.
Here, I will present our novel numerical method of implementing SA in the hybrid Eulerian-Lagrangian framework that already accounts for DSA in the presence of radiative processes like synchrotron and IC emission. The focus would be to showcase the interplay between the particle acceleration process due to shocks and turbulence. Further, I will also discuss the application of these acceleration mechanisms in governing the characteristic of the non-thermal emission from radio-lobes of AGN jets.|