Kinetic equilibrium of nonlinear electromagnetic waves in electron-positron-ion magnetoplasmas

1989 ◽  
Vol 152 (2) ◽  
pp. 181-190 ◽  
Author(s):  
F. B. Rizzato ◽  
R. S. Schneider ◽  
D. Dillenburg
Keyword(s):  
Electromagnetic Waves ◽  
Electron Positron ◽  
Kinetic Equilibrium

Nonlinear interaction of intense electromagnetic waves with a magnetoactive electron-positron-ion plasma

2013 ◽  
Vol 20 (8) ◽  
pp. 082123 ◽  
Author(s):  
S. M. Khorashadizadeh ◽  
E. Rastbood ◽  
H. Zeinaddini Meymand ◽  
A. R. Niknam
Keyword(s):  
Nonlinear Interaction ◽  
Electromagnetic Waves ◽  
Ion Plasma ◽  
Electron Positron

scholarly journals Electromagnetic albedo of Quantum Black Holes

2021 ◽  
Vol 2021 (7) ◽  
Author(s):  
Wan Zhen Chua ◽  
Niayesh Afshordi
Keyword(s):  
Black Hole ◽  
Electromagnetic Waves ◽  
Loop Correction ◽  
Quantum Black Hole ◽  
Long Wavelength ◽  
Electron Positron ◽  
Low Energies ◽  
The One ◽  
Electron Photon ◽  
Plasma Dispersion

Abstract We compute the albedo (or reflectivity) of electromagnetic waves off the electron-positron Hawking plasma that surrounds the horizon of a Quantum Black Hole. We adopt the “modified firewall conjecture” for fuzzballs [1, 2], where we consider significant electromagnetic interaction around the horizon. While prior work has treated this problem as an electron-photon scattering process, we find that the incoming quanta interact collectively with the fermionic excitations of the Hawking plasma at low energies. We derive this via two different methods: one using relativistic plasma dispersion relation, and another using the one-loop correction to photon propagator. Both methods find that the reflectivity of long wavelength photons off the Hawking plasma is significant, contrary to previous claims. This leads to the enhancement of the electromagnetic albedo for frequencies comparable to the Hawking temperature of black hole horizons in vacuum. We comment on possible observable consequences of this effect.

scholarly journals Bunch Expansion as a Cause for Pulsar Radio Emissions

2021 ◽  
Vol 923 (1) ◽  
pp. 99
Author(s):  
Jan Benáček ◽  
Patricio A. Muñoz ◽  
Jörg Büchner
Keyword(s):  
Electric Field ◽  
Electromagnetic Waves ◽  
Plasma Heating ◽  
Plasma Temperature ◽  
Weighting Factor ◽  
Field Energy ◽  
Initial Kinetic Energy ◽  
Pulsar Radio ◽  
Electron Positron ◽  
Pic Code

Abstract Electromagnetic waves due to electron–positron clouds (bunches), created by cascading processes in pulsar magnetospheres, have been proposed to explain the pulsar radio emission. In order to verify this hypothesis, we utilized for the first time Particle-in-Cell (PIC) code simulations to study the nonlinear evolution of electron–positron bunches dependant on the initial relative drift speeds of electrons and positrons, plasma temperature, and distance between the bunches. For this sake, we utilized the PIC code ACRONYM with a high-order field solver and particle weighting factor, appropriate to describe relativistic pair plasmas. We found that the bunch expansion is mainly determined by the relative electron–positron drift speed. Finite drift speeds were found to cause the generation of strong electrostatic superluminal waves at the bunch density gradients that reach up to E ∼ 7.5 × 105 V cm−1 (E/(m e c ω p e −1) ∼ 4.4) and strong plasma heating. As a result, up to 15% of the initial kinetic energy is transformed into the electric field energy. Assuming the same electron and positron distributions, we found that the fastest (in the bunch reference frame) particles of consecutively emitted bunches eventually overlap in momentum (velocity) space. This overlap causes two-stream instabilities that generate electrostatic subluminal waves with electric field amplitudes reaching up to E ∼ 1.9 × 104 V cm−1 (E/(m e c ω p e −1) ∼ 0.11). We found that in all simulations the evolution of electron–positron bunches may lead to the generation of electrostatic superluminal or subluminal waves, which, in principle, can be behind the observed electromagnetic emissions of pulsars in the radio wave range.

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