scholarly journals Computational Study of Magnetic Field Amplification in Laser-Produced Shock Waves Relevant to Supernova Remnants

2016 ◽  
Vol 688 ◽  
pp. 012035
Author(s):  
Ayako Ishii ◽  
Shiori Kishita ◽  
Naofumi Ohnishi ◽  
Yasuhiro Kuramitsu ◽  
Taichi Morita ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Shock Waves ◽  
Supernova Remnants ◽  
Computational Study ◽  
Field Amplification

scholarly journals Turbulent Magnetic Field Amplification behind Strong Shock Waves in GRB and SNR

2011 ◽  
Vol 7 (S279) ◽  
pp. 335-336
Author(s):  
Tsuyoshi Inoue
Keyword(s):  
Magnetic Field ◽  
Shock Wave ◽  
Shock Waves ◽  
Supernova Remnants ◽  
Gamma Ray ◽  
Three Dimensional ◽  
Strong Shock ◽  
Field Amplification ◽  
Field Lines ◽  
Strong Shock Waves

AbstractUsing three-dimensional (special relativistic) magnetohydrodynamics simulations, the amplification of magnetic field behind strong shock wave is studied. In supernova remnants and gamma-ray bursts, strong shock waves propagate through an inhomogeneous density field. When the shock wave hit a density bump or density dent, the Richtmyer-Meshkov instability is induced that cause a deformation of the shock front. The deformed shock leaves vorticity behind the shock wave that amplifies the magnetic field due to the stretching of field lines.

scholarly journals Magnetic field amplification in Tycho and other shell-type supernova remnants

2005 ◽  
Vol 444 (3) ◽  
pp. 893-893 ◽  
Author(s):  
H. J. Völk ◽  
E. G. Berezhko ◽  
L. T. Ksenofontov
Keyword(s):  
Magnetic Field ◽  
Supernova Remnants ◽  
Field Amplification ◽  
Shell Type

scholarly journals Evolution of magnetic field in a weakly relativistic counterstreaming inhomogeneous e−/e+ plasmas

2020 ◽  
Vol 38 (3) ◽  
pp. 181-187
Author(s):  
Sandeep Kumar ◽  
Y. K. Kim ◽  
T. Kang ◽  
Min Sup Hur ◽  
Moses Chung
Keyword(s):  
Magnetic Field ◽  
Supernova Remnants ◽  
Gamma Ray ◽  
Inhomogeneous Plasma ◽  
Density Fluctuations ◽  
Weibel Instability ◽  
Thermal Anisotropy ◽  
Field Amplification ◽  
Plasma Distribution ◽  
The Magnetic Field

AbstractThe nonlinear evolution of electron Weibel instability in a symmetric, counterstream, unmagnetized electron–positron e−/e+ plasmas is studied by a 2D particle-in-cell (PIC) method. The magnetic field is produced and amplified by the Weibel instability, which extracts energy from the plasma anisotropy. A weakly relativistic drift velocity of 0.5c is considered for two counterstreaming e−/e+ plasma flows. Simulations show that in a homogeneous e−/e+ plasma distribution, the magnetic field amplifies exponentially in the linear regime and rapidly decays after saturation. However, in the case of inhomogeneous e−/e+ plasma distribution, the magnetic field re-amplifies at post-saturation. We also find that the amount of magnetic field amplification at post-saturation depends on the strength of the density inhomogeneity of the upstream plasma distribution. The temperature calculation shows that the finite thermal anisotropy exists in the case of an inhomogeneous plasma distribution which leads to the second-stage magnetic field amplification after the first saturation. Such density inhomogeneities are present in a variety of astrophysical sources: for example, in supernova remnants and gamma-ray bursts. Therefore, the present analysis is very useful in understanding these astrophysical sources, where anisotropic density fluctuations are very common in the downstream region of the relativistic shocks and the widely distributed magnetic field.

scholarly journals Magnetic field amplification in Tycho and other shell-type supernova remnants

2005 ◽  
Vol 433 (1) ◽  
pp. 229-240 ◽  
Author(s):  
H. J. Völk ◽  
E. G. Berezhko ◽  
L. T. Ksenofontov
Keyword(s):  
Magnetic Field ◽  
Supernova Remnants ◽  
Field Amplification ◽  
Shell Type
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