Three-dimensional simulations of the non-thermal broadband emission from young supernova remnants including efficient particle acceleration
Abstract
Supernova remnants are believed to be major contributors to Galactic cosmic rays. In this paper, we explore how the non-thermal emission from young remnants can be used to probe the production of energetic particles at the shock (both protons and electrons). Our model couples hydrodynamic simulations of a supernova remnant with a kinetic treatment of particle acceleration. We include two important back-reaction loops upstream of the shock: energetic particles can (1) modify the flow structure and (2) amplify the magnetic field. As the latter process is not fully understood, we use different limit cases that encompass a wide range of possibilities. We follow the history of the shock dynamics and of the particle transport downstream of the shock, which allows us to compute the non-thermal emission from the remnant at any given age. We do this in three dimensions, in order to generate projected maps that can be compared with observations. We observe that completely different recipes for the magnetic field can lead to similar modifications of the shock structure, although to very different configurations of the field and particles. We show how this affects the emission patterns in different energy bands, from radio to X-rays and γ-rays. High magneticmore »
- Authors:
-
- Department of Physics and Astronomy, University of Manitoba, Winnipeg, MB R3T 2N2 (Canada)
- Laboratoire AIM (CEA/Irfu, CNRS/INSU, Université Paris VII), CEA Saclay, bât. 709, F-91191 Gif sur Yvette (France)
- Publication Date:
- OSTI Identifier:
- 22356485
- Resource Type:
- Journal Article
- Journal Name:
- Astrophysical Journal
- Additional Journal Information:
- Journal Volume: 789; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCELERATION; CONFIGURATION; COSMIC RADIATION; DECAY; ELECTRONS; EMISSION; GALAXIES; GAMMA RADIATION; MAGNETIC FIELDS; MODIFICATIONS; PROTONS; RESONANCE IONIZATION MASS SPECTROSCOPY; SIMULATION; SUPERNOVA REMNANTS; SYNCHROTRON RADIATION; THREE-DIMENSIONAL CALCULATIONS; X RADIATION
Citation Formats
Ferrand, Gilles, Safi-Harb, Samar, and Decourchelle, Anne. Three-dimensional simulations of the non-thermal broadband emission from young supernova remnants including efficient particle acceleration. United States: N. p., 2014.
Web. doi:10.1088/0004-637X/789/1/49.
Ferrand, Gilles, Safi-Harb, Samar, & Decourchelle, Anne. Three-dimensional simulations of the non-thermal broadband emission from young supernova remnants including efficient particle acceleration. United States. https://doi.org/10.1088/0004-637X/789/1/49
Ferrand, Gilles, Safi-Harb, Samar, and Decourchelle, Anne. 2014.
"Three-dimensional simulations of the non-thermal broadband emission from young supernova remnants including efficient particle acceleration". United States. https://doi.org/10.1088/0004-637X/789/1/49.
@article{osti_22356485,
title = {Three-dimensional simulations of the non-thermal broadband emission from young supernova remnants including efficient particle acceleration},
author = {Ferrand, Gilles and Safi-Harb, Samar and Decourchelle, Anne},
abstractNote = {Supernova remnants are believed to be major contributors to Galactic cosmic rays. In this paper, we explore how the non-thermal emission from young remnants can be used to probe the production of energetic particles at the shock (both protons and electrons). Our model couples hydrodynamic simulations of a supernova remnant with a kinetic treatment of particle acceleration. We include two important back-reaction loops upstream of the shock: energetic particles can (1) modify the flow structure and (2) amplify the magnetic field. As the latter process is not fully understood, we use different limit cases that encompass a wide range of possibilities. We follow the history of the shock dynamics and of the particle transport downstream of the shock, which allows us to compute the non-thermal emission from the remnant at any given age. We do this in three dimensions, in order to generate projected maps that can be compared with observations. We observe that completely different recipes for the magnetic field can lead to similar modifications of the shock structure, although to very different configurations of the field and particles. We show how this affects the emission patterns in different energy bands, from radio to X-rays and γ-rays. High magnetic fields (>100 μG) directly impact the synchrotron emission from electrons, by restricting their emission to thin rims, and indirectly impact the inverse Compton emission from electrons and also the pion decay emission from protons, mostly by shifting their cut-off energies to respectively lower and higher energies.},
doi = {10.1088/0004-637X/789/1/49},
url = {https://www.osti.gov/biblio/22356485},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 789,
place = {United States},
year = {Tue Jul 01 00:00:00 EDT 2014},
month = {Tue Jul 01 00:00:00 EDT 2014}
}