scholarly journals Fundamentals of collisionless shocks for astrophysical application, 1. Non-relativistic shocks

2009 ◽  
Vol 17 (4) ◽  
pp. 409-535 ◽  
Author(s):  
R. A. Treumann
Keyword(s):  
Collisionless Shocks ◽  
Astrophysical Application ◽  
Relativistic Shocks

scholarly journals Constraining the magnetic field structure in collisionless relativistic shocks with a radio afterglow polarization upper limit in GW 170817

2019 ◽  
Vol 491 (4) ◽  
pp. 5815-5825 ◽  
Author(s):  
Ramandeep Gill ◽  
Jonathan Granot
Keyword(s):  
Magnetic Field ◽  
Gamma Ray ◽  
Ambient Medium ◽  
Radial Profile ◽  
Skin Depth ◽  
Relativistic Electrons ◽  
Collisionless Shocks ◽  
Particle In Cell ◽  
Upper Limit ◽  
Relativistic Shocks

ABSTRACT Gamma-ray burst (GRB) afterglow arises from a relativistic shock driven into the ambient medium, which generates tangled magnetic fields and accelerates relativistic electrons that radiate the observed synchrotron emission. In relativistic collisionless shocks the post-shock magnetic field $\boldsymbol {B}$ is produced by the two-stream and/or Weibel instabilities on plasma skin-depth scales (c/ωp), and is oriented predominantly within the shock plane (B⊥; transverse to the shock normal, $\hat{\boldsymbol {n}}_{\rm {sh}}$), and is often approximated to be completely within it ($B_\parallel \equiv \hat{\boldsymbol {n}}_{\rm {sh}}\, \cdot \, \boldsymbol {B}=0$). Current 2D/3D particle-in-cell simulations are limited to short time-scales and box sizes ≲104(c/ωp) ≪ R/Γsh much smaller than the shocked region’s comoving width, and hence cannot probe the asymptotic downstream $\boldsymbol {B}$ structure. We constrain the latter using the linear polarization upper limit, $\vert \Pi \vert \lt 12{{\ \rm per\ cent}}$, on the radio afterglow of GW $170817$ / GRB 170817A. Afterglow polarization depends on the jet’s angular structure, our viewing angle, and the $\boldsymbol {B}$ structure. In GW $170817$ / GRB 170817A the latter can be tightly constrained since the former two are well-constrained by its exquisite observations. We model $\boldsymbol {B}$ as an isotropic field in 3D that is stretched along $\hat{\boldsymbol {n}}_{\rm {sh}}$ by a factor ξ ≡ $B_\parallel $/B⊥, whose initial value ξf ≡ $B_\parallel,$f/B⊥, f describes the field that survives downstream on plasma scales ≪R/Γsh. We calculate Π(ξf) by integrating over the entire shocked volume for a Gaussian or power-law core-dominated structured jet, with a local Blandford-McKee self-similar radial profile (used for evolving ξ downstream). We find that independent of the exact jet structure, $\boldsymbol {B}$ has a finite, but initially sub-dominant, parallel component: 0.57 ≲ ξf ≲ 0.89, making it less anisotropic. While this motivates numerical studies of the asymptotic $\boldsymbol {B}$ structure in relativistic collisionless shocks, it may be consistent with turbulence amplified magnetic field.

scholarly journals Generation and decay of the magnetic field in collisionless shocks

2016 ◽  
Vol 12 (S324) ◽  
pp. 62-65
Author(s):  
Mikhail Garasev ◽  
Evgeny Derishev
Keyword(s):  
Magnetic Field ◽  
Large Scale ◽  
Field Energy ◽  
Magnetic Field Generation ◽  
Collisionless Shocks ◽  
Particle In Cell ◽  
Magnetic Field Energy ◽  
Relativistic Shocks ◽  
Continuous Injection ◽  
The Magnetic Field

AbstractWe present the results of numerical particle-in-cell (PIC) simulations of the magnetic field generation and decay in the upstream of collisionless shocks. We use the model, where the magnetic field in the incoming flow is generated by continuous injection of anisotropic electron-positron pairs. We found that the continuous injection of anisotropic plasma in the upstream of the shock-wave generates the large-scale, slowly decaying magnetic field that is later amplified during the passage of the shock front. In our simulations the magnetic field energy reached ~0.01 of the equipartition value, after that it slowly decays on the time scale proportional to the duration of the injection in the upstream. Thus, the magnetic field survives for a sufficiently long time, and supports efficient synchrotron radiation from relativistic shocks, e.g., in GRBs.

scholarly journals Monte Carlo simulations of fast Newtonian and mildly relativistic shock breakout from a stellar wind

2020 ◽  
Vol 499 (4) ◽  
pp. 4961-4971
Author(s):  
Hirotaka Ito ◽  
Amir Levinson ◽  
Ehud Nakar
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Simulations ◽  
Stellar Wind ◽  
Compact Star ◽  
Strong Dependence ◽  
Shock Velocity ◽  
Light Curves ◽  
Ultraviolet Emission ◽  
Relativistic Shocks ◽  
Strong Explosion

ABSTRACT Strong explosion of a compact star surrounded by a thick stellar wind drives a fast (>0.1c) radiation mediated shock (RMS) that propagates in the wind, and ultimately breaks out gradually once photons start escaping from the shock transition layer. In exceptionally strong or aspherical explosions, the shock velocity may even be relativistic. The properties of the breakout signal depend on the dynamics and structure of the shock during the breakout phase. Here we present, for the first time, spectra and light curves of the breakout emission of fast Newtonian and mildly relativistic shocks, that were calculated using self-consistent Monte Carlo simulations of finite RMS with radiative losses. We find a strong dependence of the νFν peak on shock velocity, ranging from ∼1 keV for vs/c = 0.1 to ∼100 keV for vs/c = 0.5, with a shift to lower energies as losses increase. For all cases studied the spectrum below the peak exhibits a nearly flat component (Fν ∼ ν0) that extends down to the break frequency below which absorption becomes important. This implies much bright optical/ultraviolet emission than hitherto expected. The computed light curves show a gradual rise over tens to hundreds of seconds for representative conditions. The application to SN 2008D/XRT 080109 and the detectability limits are also discussed. We predict a detection rate of about one per year with eROSITA.

scholarly journals ELECTRON INJECTION BY WHISTLER WAVES IN NON-RELATIVISTIC SHOCKS

2011 ◽  
Vol 733 (1) ◽  
pp. 63 ◽  
Author(s):  
Mario A. Riquelme ◽  
Anatoly Spitkovsky
Keyword(s):  
Electron Injection ◽  
Whistler Waves ◽  
Relativistic Shocks
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