# Modeling Gamma-Ray Burst X-Ray Flares within the Internal Shock Model

## TL;DR

This paper presents a shell model within the internal shock framework to simulate and explain the observed X-ray flares in gamma-ray burst afterglows, linking flare activity to central engine reactivation.

## Contribution

The study introduces a novel shell model code that reproduces X-ray flare phenomenology and constrains central engine activity based on observational data.

## Key findings

- X-ray flare properties can be explained by internal shocks from multiple shells.
- The model links flare timing and width to central engine activity.
- Reactivation of the central engine occurs multiple times with decreasing energy.

## Abstract

X-ray afterglow light curves have been collected for over 400 Swift gamma-ray bursts with nearly half of them having X-ray flares superimposed on the regular afterglow decay. Evidence suggests that gamma-ray prompt emission and X-ray flares share a common origin and that at least some flares can only be explained by long-lasting central engine activity. We have developed a shell model code to address the question of how X-ray flares are produced within the framework of the internal shock model. The shell model creates randomized GRB explosions from a central engine with multiple shells and follows those shells as they collide, merge and spread, producing prompt emission and X-ray flares. We pay special attention to the time history of central engine activity, internal shocks, and observed flares, but do not calculate the shock dynamics and radiation processes in detail. Using the empirical E_p - E_iso (Amati) relation with an assumed Band function spectrum for each collision and an empirical flare temporal profile, we calculate the gamma-ray (Swift/BAT band) and X-ray (Swift/XRT band) lightcurves for arbitrary central engine activity and compare the model results with the observational data. We show that the observed X-ray flare phenomenology can be explained within the internal shock model. The number, width and occurring time of flares are then used to diagnose the central engine activity, putting constraints on the energy, ejection time, width and number of ejected shells. We find that the observed X-ray flare time history generally reflects the time history of the central engine, which reactivates multiple times after the prompt emission phase with progressively reduced energy...