The interaction phase of engine-driven explosions and high-energy winds

TL;DR

This paper systematically studies the evolution of wind-driven bubbles in astrophysical systems, analyzing their phases, relaxation timescales, and similarity solutions through analytic and simulation methods.

Contribution

It provides a comprehensive analysis of the adiabatic phases of wind-driven outflows into power-law density profiles, including new quantitative insights and validation of similarity solutions.

Findings

Interaction solutions are reached within a few dynamical times.

Similarity solutions accurately describe the flow until the reverse shock becomes non-thin.

For density profiles with n<2, the flow converges to a specific energy-conserving scaling.

Abstract

Wide-angle outflows, or winds, are associated with a broad range of astrophysical systems, including protostars, massive stars, X-ray binaries, tidal disruption events (TDEs), luminous fast blue optical transients (LFBOTs), and starburst galaxies. When these winds first ``turn on," they inflate a ``bubble" into their surroundings, bounded by two shocks and a contact discontinuity, and evolve through distinct adiabatic phases prior to the onset of significant radiative cooling. For sufficiently overdense ejecta, the flow quickly relaxes into an interaction-dominated similarity state at early times and later enters an energy-conserving regime. We present a systematic study of these phases for adiabatic winds expanding into power-law density profiles $\rho \propto r^{-n}$ with $0 \leq n \leq 2$. Using analytic scalings together with one-dimensional shock-capturing hydrodynamic simulations, we quantify both the relaxation timescales and the accuracy with which the corresponding similarity solutions reproduce the fluid velocity, density, and pressure throughout the shocked bubble. We show that the interaction solutions are attained within only a few dynamical times and remain valid until the reverse-shocked shell is no longer thin relative to the forward-shocked shell, corresponding in practice to an instantaneous overdensity of order unity. For $n < 2$, the flow subsequently converges to the generalized energy-conserving scaling $R_s \propto t^{3/(5-n)}$, while the special case $n=2$ exhibits a single persistent similarity state. We discuss the durations and implications of these phases for stellar and galactic outflows, TDEs, and LFBOTs.