Hadronic re-acceleration at the Crab pulsar wind termination shock as a source of PeV gamma-rays

Spencer S, Mitchell A, Reville B (2023)

Publication Type: Conference contribution

Publication year: 2023

Book Volume: 444

Event location: Nagoya JP

DOI: 10.22323/1.444.0690

Abstract

Recent results from LHAASO and Tibet ASγ suggest that the Crab Nebula’s gamma-ray spectrum extends to the PeV energy range, however the production mechanisms of this highest energy emission remain unclear. It has been postulated that a secondary component of hadronic emission could explain the highest energy gamma-ray flux points, however the origin and acceleration mechanism for this hadronic population has yet to be explained. We postulate one scenario in which hadrons diffuse over time into the Crab pulsar wind nebula from the surrounding supernova ejecta, and are subsequently re-accelerated by the pulsar wind termination shock. We present results of direct particle transport simulations (including radial evolution) to determine if this scenario is viable over the lifetime of the Crab system.

Authors with CRIS profile

Samuel Spencer Lehrstuhl für Physik Alison Mitchell Lehrstuhl für Physik

Involved external institutions

University of Oxford GB United Kingdom (GB)

How to cite

APA:

Spencer, S., Mitchell, A., & Reville, B. (2023). Hadronic re-acceleration at the Crab pulsar wind termination shock as a source of PeV gamma-rays. In Proceedings of the 38th International Cosmic Ray Conference (ICRC2023). Nagoya, JP.

MLA:

Spencer, Samuel, Alison Mitchell, and Brian Reville. "Hadronic re-acceleration at the Crab pulsar wind termination shock as a source of PeV gamma-rays." Proceedings of the 38th International Cosmic Ray Conference (ICRC2023), Nagoya 2023.

BibTeX: Download