Propagation of GRB Relativistic Jets in AGN Disks and Its Implication for GRB Detection

Abstract

The accretion disks of supermassive black holes (SMBHs) harboring in active galactic nuclei (AGN) are considered to be an ideal site for producing different types of gamma-ray bursts (GRBs). The detectability of these GRB phenomena hidden in AGN disks is highly dependent on the dynamical evolution of the GRB relativistic jets. By investigating the reverse and forward shock dynamics due to the interaction between the jets and AGN disk material, we find that the relativistic jets can successfully break out from the disks only for a sufficiently high luminosity and a long enough duration. In comparison, relatively normal GRB jets are inclined to be choked in the disks, unless the GRBs occur near an SMBH with relatively low mass (e.g., $\sim 10^6{M}_{\odot }$). For the choked jets, unlike normal GRB prompt and afterglow emission, we can only expect to detect emission from the forward shock when the shock is very close to the edge of the disks, i.e., the shock breakout emission and subsequent cooling of the shock.

9 pages, 6 figures

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• The puzzling long GRB 191019A: Evidence for Kilonova Light
• Observational Properties of Thermal Emission from Relativistic Jets Embedded in AGN Disks
• The origin channels of hierarchical binary black hole mergers in the LIGO-Virgo-KAGRA O1, O2, and O3 runs
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• Propagation of Precessing Jet in Envelope of Tidal Disruption Events
• The Use of Binary Black Holes Merging in AGN Disks for Hubble Constant Measurements