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Inverse of proton acceleration and cooling timescales as a function of proton energy in the jet head frame for a classical LGRB (left panel) and SGRB (right panel). Acceleration (red solid), photomeson production (pγ, blue dashed), BetheHeitler pair production (blue dotted), hadronuclear scattering (pp, blue dashed-dotted), inverse-Compton (IC, green dashed), synchrotron radiation (green dotted), and adiabatic cooling (green dashed-dotted) processes are considered.
Source publication
Both long-duration gamma-ray bursts (LGRBs) from core collapse of massive stars and short-duration GRBs (SGRBs) from mergers of binary neutron star (BNS) or neutron star--black hole (NSBH) are expected to occur in the accretion disk of active galactic nuclei (AGNs). We show that GRB jets embedded in the migration traps of AGN disks are promised to...
Context in source publication
Context 1
... the timescale that protons to lose energy due to adiabatic cooling is t p,ada = r stall /cΓ h . We present the acceleration and cooling timescales of a choked LGRB and SGRB jet in an AGN disk in Fig. 2. For both cases, pp scattering would dominate the cooling process for lowenergy protons. Bethe-Heitler process leads and suppresses neutrino production if the energy of protons falls within the range of 0.5 TeV p 20 TeV. At higher energies, the dominant cooling mechanism for protons is pγ interaction, which also limits the maximum ...
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