Hyperaccretion-driven relativistic jets from massive collapsars in active galactic nucleus disks

TL;DR

This paper investigates how hyperaccretion-driven relativistic jets from massive collapsars in AGN disks can produce observable gamma-ray bursts, influenced by progenitor star properties and disk environment, with implications for future detections.

Contribution

It introduces a model linking massive star properties, jet breakout conditions, and observable GRB signatures in AGN disks, highlighting the role of hyperaccretion in jet longevity and detectability.

Findings

Low metallicity stars can produce longer-lasting jets.

Jets may break out from AGN disks under certain conditions.

Detectability of these GRBs by Swift and Einstein Probe is discussed.

Abstract

The observable characteristics of gamma-ray bursts (GRBs) embedded in the accretion disk of active galactic nuclei (AGNs) are mainly determined by the jet propagation within the disk. In the massive collapsar scenario, we consider that the mass and metallicity of progenitor stars can significantly affect the jet durations and luminosities, which in turn influence whether the jet can break out from AGN disks. For the cases with low metallicity, massive stars tend to keep their massive envelopes. Thus the hyperaccretion of these envelopes onto the newborn black holes (BHs) can prolong the activity duration of the central engine, thereby allowing the jets to potentially break out from the disks. For successful jets, we further study their prompt emission and afterglows for different supermassive BHs and locations and discuss the detectability of these signals by instruments such as \emph{Swift} and Einstein Probe. Future related observations will help constrain the structure, components, and evolutionary history of AGN disks and the massive stars embedded within them.