Ultra-relativistic geometrical shock dynamics and vorticity

TL;DR

This paper extends geometrical shock dynamics to ultra-relativistic shocks in astrophysical contexts, deriving approximate equations, comparing with numerical solutions, and analyzing relativistic vorticity and circulation.

Contribution

It adapts nonrelativistic geometrical shock dynamics to ultra-relativistic regimes and explores vorticity behavior in such flows, providing exact solutions and comparisons.

Findings

Exact solutions for self-similar shocks with power-law density profiles.

Relativistic vorticity changes only at shocks, not in smooth flow regions.

Good agreement between approximate equations and numerical hydrodynamic solutions.

Abstract

Geometrical shock dynamics, also called CCW theory, yields approximate equations for shock propagation in which only the conditions at the shock appear explicitly; the post-shock flow is presumed approximately uniform and enters implicitly via a Riemann invariant. The nonrelativistic theory, formulated by G. B. Whitham and others, matches many experimental results surprisingly well. Motivated by astrophysical applications, we adapt the theory to ultra-relativistic shocks advancing into an ideal fluid whose pressure is negligible ahead of the shock, but one third of its proper energy density behind the shock. Exact results are recovered for some self-similar cylindrical and spherical shocks with power-law pre-shock density profiles. Comparison is made with numerical solutions of the full hydrodynamic equations. We review relativistic vorticity and circulation. In an ultrarelativistic ideal fluid, circulation can be defined so that it changes only at shocks, notwithstanding entropy gradients in smooth parts of the flow.