Escape of cosmic rays from perpendicular shocks in the interstellar magnetic field
arXiv:2107.05820 · doi:10.1103/PhysRevD.104.083028
Abstract
We investigate the escape process from a perpendicular shock region of a spherical shock in the interstellar medium (ISM). The diffusive shock acceleration in the perpendicular shock of supernova remnants (SNRs) has been expected to accelerate cosmic rays (CRs) to the PeV scale without an upstream magnetic field amplification. We estimate the maximum energy of CRs limited by the escape from the perpendicular shock region. By performing test particle simulations, we confirm the theoretical estimation, showing that the escape-limited maximum energy in the perpendicular shock is several 10 TeV for the typical type Ia SNRs. Therefore, in order for SNRs in the ISM to accelerate CRs to the PeV scale, an upstream magnetic field amplification is needed. The characteristic energy scale of several 10 TeV could be the origin of the spectral break around 10 TeV, which was reported by recent direct CR observations. In addition, we show that, in the free expansion phase, the rapid perpendicular shock acceleration works on about 20% area of the whole shock surface, which is larger than the size of the superluminal shock region. We also discuss the escape of CR electrons from the perpendicular shock.
arXiv comment9 pages, 4 figures, accepted for publication in PRD
References in corpus (39)
- Acceleration of petaelectronvolt protons in the Galactic Centre
- Fine Structures of Shock of SN 1006 with the Chandra Observation
- Measurement of the cosmic-ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite
- Proton and Helium Spectra from the CREAM-III Flight
- First Detection of sub-PeV Diffuse Gamma Rays from the Galactic Disk: Evidence for Ubiquitous Galactic Cosmic Rays beyond PeV Energies
- On the spectrum of high-energy cosmic rays produced by supernova remnants in the presence of strong cosmic-ray streaming instability and wave dissipation
- Turbulence and Magnetic Field Amplification in Supernova Remnants: Interactions Between A Strong Shock Wave and Multi-Phase Interstellar Medium
- Limits on diffusive shock acceleration in supernova remnants in the presence of cosmic-ray streaming instability and wave dissipation
- Non-linear Study of Bell's Cosmic Ray Current-driven Instability
- Gamma rays from molecular clouds illuminated by cosmic rays escaping from interacting supernova remnants
- Measurement of the cosmic ray helium energy spectrum from 70 GeV to 80 TeV with the DAMPE space mission
- Diffusive Shock Acceleration with Magnetic Amplification by Non-resonant Streaming Instability in SNRs
- Confirmation of strong magnetic field amplification and nuclear cosmic ray acceleration in SN 1006
- Production of Magnetic Turbulence by Cosmic Rays Drifting Upstream of Supernova Remnant Shocks
- Extended Very-High-Energy Gamma-Ray Emission Surrounding PSR J0622 + 3749 Observed by LHAASO-KM2A
- Escape-limited Model of Cosmic-ray Acceleration Revisited
- Non-linear Particle Acceleration in Oblique Shocks
- Chandra Observations of A Galactic Supernova Remnant Vela Jr.: A New Sample of Thin Filaments Emitting Synchrotron X-Rays
- A new universal cosmic-ray knee near the magnetic rigidity 10 TV with the NUCLEON space observatory
- Potential PeVatron supernova remnant G106.3+2.7 seen in the highest-energy gamma rays
- The Effect of Large Scale Magnetic Turbulence on the Acceleration of Electrons by Perpendicular Collisionless Shocks
- Two-Dimensional particle-in-cell simulations of the nonresonant, cosmic-ray driven instability in SNR shocks
- Escape of cosmic-ray electrons from supernova remnants
- HAWC J2227+610 and its association with G106.3+2.7, a new potential Galactic PeVatron
- Diffusive Shock Re-Acceleration
- Gamma-ray emission of accelerated particles escaping a supernova remnant in a molecular cloud
- The shape of the cosmic ray proton spectrum
- Evidence of 200 TeV photons from HAWC J1825-134
- Turbulent amplification of magnetic field driven by dynamo effect at rippled shocks
- Evidence that Ultra-High-Energy Gamma Rays are a Universal Feature Near Powerful Pulsars
- Rapid cosmic-ray acceleration at perpendicular shocks in supernova remnants
- Pulsar Wind Nebulae inside Supernova Remnants as Cosmic-Ray PeVatrons
- Effects of Leakage Neutral Particles on Shocks
- Effects of Neutral Particles on Modified Shocks at Supernova Remnants
- Magnetic field amplification by collisionless shocks in partially ionized plasmas
- Injection to rapid diffusive shock acceleration at perpendicular shocks in partially ionized plasmas
- Simulations of Collisionless Perpendicular Shocks in Partially Ionized Plasmas
- Acoustic instability in the neutral precursor region of collisionless shocks propagating into partially ionized plasmas
- Fast Particle Acceleration at Perpendicular Shocks with Uniform Upstream Magnetic Field and Strong Downstream Turbulence