The Multiband Emission of the two-component Gamma-Ray Burst jet influenced by progenitor winds within the Accretion Disk of Active Galactic Nuclei

TL;DR

This paper models the multiband emission of two-component GRB jets within AGN disks, considering progenitor winds and cavities, to understand jet propagation, emission signatures, and aid in GRB classification.

Contribution

It introduces a detailed model of two-component GRB jets in AGN environments, accounting for wind-influenced cavities and predicts observable signatures for different GRB types.

Findings

Long GRB jets are choked by cavities, with emissions similar to no-cavity cases.

Cocoon breakout emissions are detectable by EP and HXMT.

Short GRB afterglows and cocoon emissions can be distinguished through joint EP and HXMT observations.

Abstract

Gamma-ray bursts (GRBs), both from merger of binary compact objects (short GRBs) and collapse of massive stars (long GRBs), are expected to occur in the dense environments, e.g., the accretion disk of active galactic nuclei (AGN). The propagating of GRB jets in such dense environment will result in multiband transients. Investigating the properties of these transients plays important roles in their identification, understanding the jet structure and constraining population of the star and compact object in AGN disks. In this work, we intend to study the propagation and emission of a two-component GRB jet (a fast narrow component and a wide slow one) in the AGN disk. We consider the influence of wind from the short and long GRB progenitors, which would reconstruct the surrounding density distribution and form a cavity in the AGN disk. We find that the long GRB jets will be choked, the dynamcis and the emission are resemble to the case without cavity. The cocoon breakout emission can be detected by EP and HXMT. For short GRBs, we expect a non-thermal afterglow emission from the narrow and wide jet (if it is more energetic than the narrow one) and a cocoon breakout emission from the choked wide jet, which can be monitored by EP and HXMT, respectively. Therefore, the joint observations by EP and HXMT might be helpful to distinguish the type of GRBs in the AGN disk and the jet components.