Pulsar Wind Nebulae inside Supernova Remnants as Cosmic-Ray PeVatrons

Abstract

We propose that cosmic-ray PeVatrons are pulsar wind nebulae (PWNe) inside supernova remnants (SNRs). The PWN initially expands into the freely expanding stellar ejecta. Then, the PWN catches up with the shocked region of the SNR, where particles can be slightly accelerated by the back and forth motion between the PWN and the SNR, and some particles diffuse into the PWN. Afterwards the PWN is compressed by the SNR, where the particles in the PWN are accelerated by the adiabatic compression. Using a Monte Carlo simulation, we show that particles accelerated by the SNR to 0.1 PeV can be reaccelerated to 1 PeV until the end of the PWN compression.

6 pages, 3 figures, 1 table, accepted for publication in MNRAS

References in corpus (3)

• Detection of the Characteristic Pion-Decay Signature in Supernova Remnants
• A Dynamical Model for the Evolution of a Pulsar Wind Nebula inside a Non-Radiative Supernova Remnant
• On the Structure and Scale of Cosmic Ray Modified Shocks

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• Very-high-energy gamma rays from cosmic rays escaping from Galactic black hole binaries
• The Potential for Hadronic Particle Acceleration in Galactic Pulsar Wind Nebulae
• The expected potential of hadronic PeVatron searches with spectral $\gamma$-ray data from the Southern Wide-field Gamma-ray Observatory
• Hadronic Re-Acceleration at the Crab Pulsar Wind Termination Shock as a Source of PeV Gamma-Rays
• Escape of cosmic rays from perpendicular shocks in the interstellar magnetic field