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Title: MODELING THE MULTI-WAVELENGTH EMISSION OF THE SHELL-TYPE SUPERNOVA REMNANT RX J1713.7-3946

Abstract

Emission mechanisms of the shell-type supernova remnant (SNR) RX J1713.7-3946 are studied with multi-wavelength observational data from the radio, X-ray, GeV {gamma}-ray, and TeV {gamma}-ray bands. A Markov Chain Monte Carlo method is employed to explore the high-dimensional model parameter space systematically. Three scenarios for the {gamma}-ray emission are investigated: the leptonic, the hadronic, and a hybrid. Thermal emission from the background plasma is also included to constrain the gas density, assuming ionization equilibrium, and a 2{sigma} upper limit of about 0.03 cm{sup -3} is obtained as far as thermal energies account for a significant fraction of the dissipated kinetic energy of the SNR shock. Although systematic errors dominate the {chi}{sup 2} of the spectral fit of all models, we find that (1) the leptonic model has the best constrained model parameters, whose values can be easily accommodated with a typical supernova, but gives a relatively poor fit to the TeV {gamma}-ray data; (2) the hybrid scenario has one more parameter than the leptonic one and improves the overall spectral fit significantly; and (3) the hadronic one, which has three more parameters than the leptonic model, gives the best fit to the overall spectrum with relatively poorly constrained model parametersmore » and very hard spectra of accelerated particles. The uncertainties of the model parameters decrease significantly if the spectral indices of accelerated electrons and protons are the same. The hybrid and hadronic models also require an energy input into high-energy protons, which seems to be too high compared with typical values for a supernova explosion. Further investigations are required to reconcile these observations with SNR theories.« less

Authors:
;  [1];  [2];  [3];  [4]
  1. Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049 (China)
  2. Department of Physics and Astronomy, University of Glasgow, Glasgow G12 8QQ (United Kingdom)
  3. Department of Physics, Yunnan University, Kunming 650091, Yunnan (China)
  4. Los Alamos National Laboratories, Los Alamos, NM 87545 (United States)
Publication Date:
OSTI Identifier:
21578367
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 735; Journal Issue: 2; Other Information: DOI: 10.1088/0004-637X/735/2/120; Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; COSMIC RADIATION; EMISSION; GAMMA RADIATION; MONTE CARLO METHOD; SIMULATION; SUPERNOVA REMNANTS; CALCULATION METHODS; COSMIC RADIO SOURCES; ELECTROMAGNETIC RADIATION; IONIZING RADIATIONS; RADIATIONS

Citation Formats

Yuan Qiang, Bi Xiaojun, Liu Siming, Fan Zhonghui, and Fryer, Christopher L. MODELING THE MULTI-WAVELENGTH EMISSION OF THE SHELL-TYPE SUPERNOVA REMNANT RX J1713.7-3946. United States: N. p., 2011. Web. doi:10.1088/0004-637X/735/2/120.
Yuan Qiang, Bi Xiaojun, Liu Siming, Fan Zhonghui, & Fryer, Christopher L. MODELING THE MULTI-WAVELENGTH EMISSION OF THE SHELL-TYPE SUPERNOVA REMNANT RX J1713.7-3946. United States. doi:10.1088/0004-637X/735/2/120.
Yuan Qiang, Bi Xiaojun, Liu Siming, Fan Zhonghui, and Fryer, Christopher L. Sun . "MODELING THE MULTI-WAVELENGTH EMISSION OF THE SHELL-TYPE SUPERNOVA REMNANT RX J1713.7-3946". United States. doi:10.1088/0004-637X/735/2/120.
@article{osti_21578367,
title = {MODELING THE MULTI-WAVELENGTH EMISSION OF THE SHELL-TYPE SUPERNOVA REMNANT RX J1713.7-3946},
author = {Yuan Qiang and Bi Xiaojun and Liu Siming and Fan Zhonghui and Fryer, Christopher L.},
abstractNote = {Emission mechanisms of the shell-type supernova remnant (SNR) RX J1713.7-3946 are studied with multi-wavelength observational data from the radio, X-ray, GeV {gamma}-ray, and TeV {gamma}-ray bands. A Markov Chain Monte Carlo method is employed to explore the high-dimensional model parameter space systematically. Three scenarios for the {gamma}-ray emission are investigated: the leptonic, the hadronic, and a hybrid. Thermal emission from the background plasma is also included to constrain the gas density, assuming ionization equilibrium, and a 2{sigma} upper limit of about 0.03 cm{sup -3} is obtained as far as thermal energies account for a significant fraction of the dissipated kinetic energy of the SNR shock. Although systematic errors dominate the {chi}{sup 2} of the spectral fit of all models, we find that (1) the leptonic model has the best constrained model parameters, whose values can be easily accommodated with a typical supernova, but gives a relatively poor fit to the TeV {gamma}-ray data; (2) the hybrid scenario has one more parameter than the leptonic one and improves the overall spectral fit significantly; and (3) the hadronic one, which has three more parameters than the leptonic model, gives the best fit to the overall spectrum with relatively poorly constrained model parameters and very hard spectra of accelerated particles. The uncertainties of the model parameters decrease significantly if the spectral indices of accelerated electrons and protons are the same. The hybrid and hadronic models also require an energy input into high-energy protons, which seems to be too high compared with typical values for a supernova explosion. Further investigations are required to reconcile these observations with SNR theories.},
doi = {10.1088/0004-637X/735/2/120},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 735,
place = {United States},
year = {2011},
month = {7}
}