Observational constraints on the maximum energies of accelerated particles in supernova remnants: low maximum energies and a large variety

Abstract

Supernova remnants (SNRs) are thought to be the most promising sources of Galactic cosmic rays. One of the principal questions is whether they are accelerating particles up to the maximum energy of Galactic cosmic rays ($\sim$ PeV). In this work, a systematic study of gamma-ray emitting SNRs is conducted as an advanced study of Suzuki et al. 2021. Our purpose is to newly measure the evolution of maximum particle energies with increased statistics and better age estimates. We model their gamma-ray spectra to constrain the particle-acceleration parameters. Two candidates of the maximum energy of freshly accelerated particles, the gamma-ray cutoff and break energies, are found to be well below PeV. We also test a spectral model that includes both the freshly accelerated and escaping particles to estimate the maximum energies more reliably, but no tighter constraints are obtained with current statistics. The average time dependences of the cutoff energy ($\propto t^{-0.81\pm 0.24}$) and break energy ($\propto t^{-0.77\pm 0.23}$) cannot be explained with the simplest acceleration condition (Bohm limit), and requires shock-ISM (interstellar medium) interaction. The average maximum energy during lifetime is found to be $\lesssim 20$ TeV $(t_{\mathrm{M}}/1\mathrm{kyr}{)}^{-0.8}$ with $t_{\mathrm{M}}$ being the age at the maximum, which reaches PeV if $t_{\mathrm{M}}\lesssim 10$ yr. The maximum energies during lifetime are suggested to have a variety of 1.1--1.8 dex from object to object. Although we cannot isolate the cause of this variety, this work provides an important clue to understand the microphysics of particle acceleration in SNRs.

28 pages, 12 figures, accepted for publication in ApJ

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• Hadronic Scenario for Galactic PeVatron LHAASO J1912+1014u Supported by Fermi-LAT $\gamma$-ray Data and FUGIN CO Data