2011/05/03 by Yutaka Fujita, Fumio Takahara, Yutaka Ohira +1 · 1 citation
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Cosmic ray #Dark Matter and Cosmic Phenomena #Diffusion #Front (military) #Galaxy #Gamma-ray bursts and supernovae #Interstellar medium #Mechanics #Molecular cloud #Physics #Shock (circulatory) #Shock wave #Shock waves in astrophysics #Stars #Supernova #Supernova remnant #astro-ph.HE
paper · pdf · doi:10.1111/j.1365-2966.2011.18980.x
Accepted for publication in MNRAS
arxiv created 2011/05/03 · openalex publication_date 2011/06/16 · arxiv updated 2015/05/28 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We study the escape of cosmic ray (CR) protons accelerated in a supernova remnant (SNR) by numerically solving a diffusion–convection equation for regions from the vicinity of the shock front to those far away from the front. We consider the amplifications of Alfvén waves generated by the escaping CR particles and their effects on CR escape into the interstellar medium (ISM). We find that the amplification of the waves significantly delays the escape of the particles even in regions far away from the shock front (on the scale of an SNR). This means that the energy spectrum of CR particles determined through γ-ray observations of molecular clouds around SNRs is seriously affected by the particle scattering by the waves.