Temporal Evolution Of Thermal Emission From Relativistically Expanding Plasma

TL;DR

This paper models the thermal emission from relativistically expanding plasma flows, showing how photon energies and flux decay over time, with implications for understanding gamma-ray burst observations.

Contribution

It introduces a detailed analytical and numerical model of photon cooling and escape in relativistic plasma outflows, highlighting the angular dependence of the photosphere and temporal decay of thermal emission.

Findings

Photon energy decreases as epsilon'(r) ~ r^{-2/3}.

Thermal flux decays as F_{BB}^{ob.} ~ t^{-2}.

Observed temperature follows T^{ob.}(t) ~ t^{-2/3} early on, then T^{-1/2} later.

Abstract

Propagation of photons in relativistically expanding plasma outflows, characterized by steady Lorentz factor Gamma is considered. Photons that are injected in regions of high optical depth are advected with the flow until they escape at the photosphere. Below the photosphere, the photons are coupled to the plasma via Compton scattering. I show here, that as a result of the slight misalignment of the scattering electrons velocity vectors, the (local) comoving photon energy decreases with radius as epsilon'(r) ~ r^{-2/3}. This mechanism dominates the photon cooling in scenarios of faster adiabatic cooling of the electrons. I then show that the photospheric radius of a relativistically expanding plasma wind strongly depends on the angle to the line of sight, theta. For theta <~ 1/Gamma, r_{ph} is theta independent, while for theta >~ 1/Gamma, r_{ph} ~ theta^2. I show that the theta dependence of the photosphere implies that for flow parameters characterizing GRBs, thermal photons originating from below the photosphere can be observed up to tens of seconds following the inner engine activity decay. I calculate the probability density function P(r,theta) of a thermal photon to escape the plasma at radius r and angle theta. Using this function, I show that following the termination of the internal photon injection mechanism, the thermal flux decreases as F_{BB}^{ob.} ~ t^{-2}, and that the decay of the photon energy with radius results in a power law decay of the observed temperature, T^{ob.}(t) ~ t^{-2/3} at early times, which changes to t^{-1/2} later. Detailed numerical results are in very good agreement with the analytical predictions. I discuss the consequences of this temporal behavior in view of the recent evidence for a thermal emission component observed during the prompt emission phase of GRBs.