The structure and evolution of relativistic jetted blast waves

We study, analytically and numerically, the structure and evolution of relativistic jetted blast waves that propagate in uniform media, such as those that generate afterglows of gamma-ray bursts. Similar to previous studies, we find that the evolution can be divided into two parts: (i) a pre-spreading phase, in which the jet core angle is roughly constant, θ_c,0, and the shock Lorentz factor along the axis, Γ_a, evolves as a part of the Blandford-Mckee solution, and (ii) a spreading phase, in which Γ_a drops exponentially with the radius and the core angle, θ_c, grows rapidly. Nevertheless, the jet remains collimated during the relativistic phase, where. θ_c(Γ_aβ_a = 1) ≃ 0.4θ^1/3_c,0. The transition between the phases occurs when Γ_a ≃ 0.2θ^-1_c,0. We find that the "wings"of jets with initial "narrow"structure (d log E_iso/d log θ < -3 outside of the core, where E_iso is isotropic equivalent energy), start evolving during the pre-spreading phase. By the spreading phase these jets evolve to a self-similar profile, which is independent of the initial structure, where in the wings Γ(θ)∝θ^-1.5 and E_iso(θ)∝θ^-2.6. Jets with initial "wide"structure roughly keep their initial profile during their entire evolution. We provide analytic description of the jet lateral profile evolution for a range of initial structures, as well as the evolution of Γ_a and θ_c. For off-axis GRBs, we present a relation between the initial jet structure and the light curve rising phase. Applying our model to GW170817, we find that initially the jet had θ_0,c = 0.4 -4.5