Non-equilibrium effects in steady relativistic $e^{+}{e}^{-}{\hat{I}}^3$ winds

Abstract

We consider an ultra-relativistic wind consisting of electron-positron pairs and photons with the principal goal of finding the asymptotic Lorentz factor ${\hat{I}}_{\infty }^3$ for zero baryon number. The wind is assumed to originate at radius $r_i$ where it has a Lorentz factor ${\hat{I}}_i^3$ and a temperature $T_i$ sufficiently high to maintain pair equilibrium. As $r$ increases, $T$ decreases and becomes less than the temperature corresponding to the electron mass $m_e$, after which non-equilibrium effects become important. Further out in the flow the optical depth $\ddot{I}„$ drops below one, but the pairs may still be accelerated by the photons until $\ddot{I}„$ falls below $\sim 2\times10^{-5} γ_{i}^{3/4}$. Radiative transfer calculations show that only at this point do the radiation flux and pressure start to deviate significantly from their blackbody values. The acceleration of the pairs increases ${\hat{I}}^3$ by a factor $\sim 45$ as compared to its value at the photosphere; it is shown to approach $γ_{\infty} \sim 1.4\times 10^3 (r_i/10^6\mbox{cm})^{1/4} γ_{i}^{3/4} T_i/m_e$.

41 pages, 9 figures. Submitted to MNRAS