Relativistic Jet Stream In The Radiation Process

The jets ejected from some object centers are popularly adopted to interpret the ultra-high energy phenomena in these objects. These jets may exist in active galaxies, galactic candidates and even gamma-ray bursts (GRBs). As shown by images from VLBI, HST, Chandra etc., the jets are highly relativistic and collimated. They produce high-luminosity emission at broad wavelengths and prominently present two components. It is always one of the most interesting fields in modern astrophysics to explore their radiative processes.In this present paper, we focus on the radiative processes of AGN, especially blazar's jets mostly discussed yet. About the jet emission, there are many models proposed based on different observational facts. However, these models are mostly discussed in an one-zone homogeneous emission region (blob). They are of course not enough to account for all special phenomena.Now many puzzling objects (such as the TeV blazers, MeV blazers and large-scale X-ray jets) have been observed. In my work, I try to resolve emissive mechanisms of these objects with an inhomogeneous jet model. In the inhomogeneous jet, the velocity is assumed to change in both longitudinal and transverse directions. We find that the velocity structures of the jet don't obviously influence synchrotron emission intensity, but seriously affect the locally intrinsic energy density of seed photons for inverse Compton (IC) radiation. The boosted energy density makes it possible to produce a much high IC luminosity as in some blazars. In the last paragraph, I also discussed the internal absorption of lowest- and highest-energy emission from jets.