2009/09/13 by V. N. Zirakashvili, F. A. Aharonian · 5 citations
Physics and Astronomy · #Acceleration #Astrophysical Phenomena and Observations #Astrophysics and Cosmic Phenomena #Electron #Gamma-ray bursts and supernovae #Hadron #Particle acceleration #Radiation #Relativistic particle #Spectral line #Supernova #Supernova remnant #astro-ph.GA #astro-ph.HE
paper · pdf · doi:10.1088/0004-637x/708/2/965
27 pages, 17 figures, submitted to ApJ
arxiv created 2009/09/13 · openalex publication_date 2009/12/16 · arxiv updated 2015/05/14 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
A new numerical code, designed for the detailed numerical treatment of nonlinear diffusive shock acceleration, is used for the modeling of particle acceleration and radiation in young supernova remnants (SNRs). The model is based on spherically symmetric hydrodynamic equations complemented with transport equations for relativistic particles. For the first time, the acceleration of electrons and protons by both forward and reverse shocks is studied through detailed numerical calculations. We model the energy spectra and spatial distributions of nonthermal emission of the young SNR RX J1713.7−3946 and compare the calculations with the spectral and morphological properties of this object obtained in broad energy band from radio to very high-energy gamma rays. We discuss the advantages and shortcomings of the so-called hadronic and leptonic models, which assume that the observed TeV gamma-ray emission is produced by accelerated protons and electrons, respectively. We discuss also a "composite" scenario when the gamma-ray flux from the main parts of the shell has inverse Compton origin, but with a non-negligible contribution of hadronic origin from dense clouds interacting with the shell.