Direct Numerical Simulations of Cosmic-ray Acceleration at Dense Circumstellar Medium: Magnetic Field Amplification by Bell Instability and Maximum Energy

Abstract

Galactic cosmic rays are believed to be accelerated at supernova remnants. However, whether supernova remnants can be Pevatrons is still very unclear. In this work we argue that PeV cosmic rays can be accelerated during the early phase of a supernova blast wave expansion in dense red supergiant winds. We solve in spherical geometry a system combining a diffusive-convection equation which treats cosmic-ray dynamics coupled to magnetohydrodynamics to follow gas dynamics. The fast shock expanding in a dense ionized wind is able to trigger the fast non-resonant streaming instability over day timescales, and energizes cosmic-rays even under the effect of p-p losses. We find that such environments make the blast wave a Pevatron, although the maximum energy depends on various parameters such as the injection rate and mass-loss rate of the winds. Multi-PeV energies can be reached if the progenitor mass loss rates are of the order of $10^{-3}$ Msun yr${}^{-1}$. It has been recently invoked that, prior to the explosion, hydrogen rich massive stars can produce enhanced mass loss rates. These enhanced rates would then favor the production of a Pevatron phase in early times after the shock breakout.

15 pages, 21 figures, accepted by the Astrophysical Journal

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• Core-collapse supernovae in dense environments -- particle acceleration and non-thermal emission
• Observational constraints on the maximum energies of accelerated particles in supernova remnants: low maximum energies and a large variety
• Leptonic non-thermal emission from supernova remnants evolving in the circumstellar magnetic field
• Early-time gamma-ray constraints on cosmic-ray acceleration in the core-collapse SN 2023ixf with the Fermi Large Area Telescope
• Diffusive shock acceleration at oblique high Mach number shocks
• Long-term evolution of non-thermal emission from Type Ia and core-collapse supernova remnants in a diversified circumstellar medium
• Microquasar jet-cocoon systems as PeVatrons
• How to turn a Supernova into a PeVatron
• Escape of cosmic rays from perpendicular shocks in the circumstellar magnetic field
• Supernova remnants in super bubbles as cosmic ray accelerators
• Interacting supernovae and where to find them