SSC Emission as the Origin of the Gamma Ray Afterglow Observed in GRB 980923

TL;DR

This paper proposes a unified model for GRB 980923's afterglow, attributing the tail to forward shock synchrotron emission and the high-energy component to SSC from the reverse shock, emphasizing the role of magnetic ejecta.

Contribution

It introduces a novel interpretation linking the gamma-ray afterglow components to specific shock emission mechanisms in a highly magnetized ejecta context.

Findings

The tail is consistent with early gamma-ray afterglow from forward shock.

The high-energy component is explained by SSC from reverse shock.

Ejecta must be highly magnetized for model consistency.

Abstract

GRB 980923 was one of the brightest bursts observed by the Burst and Transient Source Experiment (BATSE). Previous studies have detected two distinct components in addition to the main prompt episode, which is well described by a Band function. The first of these is a tail with a duration of approx. 400s, while the second is a high-energy component lasting approx. 2s. We summarize the observations, and argue for a unified model in which the tail can be understood as the early gamma-ray afterglow from forward shock synchrotron emission, while the high-energy component arises from synchrotron self-Comtpon (SSC) from the reverse shock. Consistency between the main assumption of thick shell emission and agreement between the observed and computed values for fluxes, break energies, starting times and spectral indices leads to a requirement that the ejecta be highly magnetized.