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We present the three-dimensional numerical simulation of jets modeled withRelativistic Radiation Hydrodynamics (RRH), that evolve across twoenvironments: i) a stratified surrounding medium and ii) a 16TI progenitormodel. We consider opacities consistent with various processes of interactionbetween the fluid and radiation, specifically, free-free, bound-free,bound-bound and electron scattering. We explore various initial conditions,with different radiation energy densities of the beam in hydrodynamical andradiation pressure dominated scenarios, considering only ultra-relativisticjets. In order to investigate the impact of the radiation field on theevolution of the jets, we compare our results with purely hydrodynamical jets.Comparing among jets driven by RRH, we find that radiation pressure dominatedjets propagate slightly faster than gas pressure dominated ones. Finally, weconstruct the luminosity Light Curves (LCs) associated with all these cases.The construction of LCs uses the fluxes of the radiation field which is fullycoupled to the hydrodynamics equations during the evolution. The mainproperties of the jets propagating on the stratified surrounding medium arethat the LCs show the same order of magnitude as the gamma-ray luminosity oftypical Long Gamma-Ray Bursts $10^{50}-10^{54}$erg/s and the difference betweenthe radiation and gas temperatures is of nearly one order of magnitude. Theproperties of jets breaking out from the progenitor star model are that the LCsare of the order of magnitude of low-luminosity GRBs $10^{46}-10^{49}$ erg/s,and in this scenario the difference between the gas and radiation temperatureis of four orders of magnitude, which is a case far from thermal equilibrium.

Evolution of jets driven by relativistic radiation hydrodynamics as Long and Low Luminosity GRBs