Radial Profiles of Non-thermal Emission from Supernova Remnant RX J1713.7-3946. (arXiv:2103.03066v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Tang_Y/0/1/0/all/0/1">Yunyong Tang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_S/0/1/0/all/0/1">Siming Liu</a>
Supernova remnant RX J1713.7-3946 (also named as G347.3-0.5) has exhibited
largest surface brightness, detailed spectral and shell-type morphology, it is
one of the brightest TeV sources. The recent H.E.S.S. observation of RX
J1713.7-3946 revealed textbf{a} broken power-law spectrum of GeV-TeV gamma-ray
spectrum and more extended gamma-ray spatial radial profile than that in the
X-ray band. Based on the diffusion shock acceleration model, we solve
spherically symmetric hydrodynamic equations and transport equations of
particles, and investigate multi-band non-thermal emission of RX J1713.7-3946
and radial profiles of its surface brightness for two selected zones in the
leptonic scenario for the $gamma$-ray emission. We found (1) the diffusion
coefficient has a weak energy-dependent, and the Kolmogorov type is favored;
(2) the magnetic field strength could vary linearly or nonlinearly with radius
for different surrounding environments because of possible turbulence in shock
downstream region, and a compressional amplification is likely to exist at the
shock front; (3) the non-thermal photons from radio to X-ray bands are
dominated by synchrotron emission from relativistic electrons, if the GeV-TeV
gamma-rays are produced by inverse Compton scattering from these electrons
interacting with the background photons, then the X-ray and gamma-ray radial
profiles can be reproduced except for the more extended $gamma$-ray emission.
Supernova remnant RX J1713.7-3946 (also named as G347.3-0.5) has exhibited
largest surface brightness, detailed spectral and shell-type morphology, it is
one of the brightest TeV sources. The recent H.E.S.S. observation of RX
J1713.7-3946 revealed textbf{a} broken power-law spectrum of GeV-TeV gamma-ray
spectrum and more extended gamma-ray spatial radial profile than that in the
X-ray band. Based on the diffusion shock acceleration model, we solve
spherically symmetric hydrodynamic equations and transport equations of
particles, and investigate multi-band non-thermal emission of RX J1713.7-3946
and radial profiles of its surface brightness for two selected zones in the
leptonic scenario for the $gamma$-ray emission. We found (1) the diffusion
coefficient has a weak energy-dependent, and the Kolmogorov type is favored;
(2) the magnetic field strength could vary linearly or nonlinearly with radius
for different surrounding environments because of possible turbulence in shock
downstream region, and a compressional amplification is likely to exist at the
shock front; (3) the non-thermal photons from radio to X-ray bands are
dominated by synchrotron emission from relativistic electrons, if the GeV-TeV
gamma-rays are produced by inverse Compton scattering from these electrons
interacting with the background photons, then the X-ray and gamma-ray radial
profiles can be reproduced except for the more extended $gamma$-ray emission.
http://arxiv.org/icons/sfx.gif
