# Relativistic simulations of long-lived reverse shocks in stratified ejecta: the origin of flares in GRB afterglows

## TL;DR

This study uses relativistic hydrodynamic simulations to demonstrate that long-lived reverse shocks in stratified ejecta can produce X-ray flares in GRB afterglows, challenging the idea that flares are solely due to late central engine activity.

## Contribution

It introduces detailed hydrodynamic simulations to model reverse shock interactions, improving upon previous ballistic models and explaining observed X-ray flare properties.

## Key findings

- Hydrodynamic simulations match observed flare timing and shape.
- Reverse shocks interacting with dense shells produce intense X-ray flares.
- Ballistic models underestimate density and miss shock reflections.

## Abstract

The X-ray light curves of the early afterglow phase from gamma-ray bursts present a puzzling variability, including flares. The origin of these flares is still debated, and often associated with a late activity of the central engine. We discuss an alternative scenario where the central engine remains short-lived and flares are produced by the propagation of a long-lived reverse shock in a stratified ejecta. Here we focus on the hydrodynamics of the shock interactions. We perform one-dimensional ultrarelativistic hydrodynamic simulations with different initial internal structure in the gamma-ray burst ejecta. We use them to extract bolometric light curves and compare with a previous study based on a simplified ballistic model. We find a good agreement between both approaches, with similar slopes and variability in the light curves, but identify several weaknesses in the ballistic model: the density is underestimated in the shocked regions, and more importantly, late shock reflections are not captured. With accurate dynamics provided by our hydrodynamic simulations, we confirm that internal shocks in the ejecta lead to the formation of dense shells. The interaction of the long-lived reverse shock with a dense shell then produces a fast and intense increase of the dissipated power. Assuming that the emission is due to the synchrotron radiation from shock-accelerated electrons, and that the external forward shock is radiatively inefficient, we find that this results in a bright flare in the X-ray lightcurve, with arrival times, shapes, and duration in agreement with the observed properties of X-ray flares in GRB afterglows.