Beam shear-Alfven instability in two-component tokamak

ON THE SPECTRUM OF THE PULSED GAMMA-RAY EMISSION OF THE CRAB PULSAR FROM 10 MeV TO 400 GeV

“…Excitation of L waves through the two-stream instability in the relativistic e − e + plasma is considered in a series of works (see, e.g., Lominadze & Mikhailovskii 1979;Usov 1987;Asseo & Melikidze 1998;Ursov & Usov 1988;Gogoberidze et al 2008), where it is assumed that the instability develops due to overlapping of the fast and slow pair plasma particles. For typical parameters of pair plasmas in pulsar magnetospheres, the growth rate of the instability is quite sufficient (see Gogoberidze et al 2008) that it inevitably permits the existence of L waves in the vicinity of the light cylinder zone.…”

“…The dispersion relation for L modes when the phase speed is very close to the speed of light, υ ph = ω L /k ≈ c, is given by (Lominadze & Mikhailovskii 1979):…”

On the spectrum of the pulsed gamma-ray emission from 10MeV to 400GeV of the Crab pulsar

“…Therefore, we assume that the Langmuir waves (L) generated via the two-stream instability at the light cylinder length-scales undergo Landau damping on the fastest beam electrons, which results in their effective acceleration. Excitation of L waves through the two-stream instability in the relativistic electron-positron plasma is considered in a series of works (see e.g., Lominadze & Mikhailovskii (1979); Usov (1987); Asseo & Melikidze (1998); Ursov & Usov (1988); Gogoberidze et al (2008)), where it is assumed that the instability develops due to overlapping of the fast and slow pair plasma particles at distances r ∼ 10 8 cm from the star surface. For typical parameters of pair plasma in the pulsar magnetospehers the growth rate of the instability is quite sufficient (see Gogoberidze et al (2008)), that inevitably provides existence of L waves in the vicinity of the light cylinder zone.…”

Generation of the electrostatic field in the pulsar magnetosphere plasma

“…For the typical parameters of the pulsar magnetosphere the charge separation scale at the light cylinder (the light cylinder is the surface, on which the azimuthal velocity equals to the speed of light V ϕ = Ωr = c) is of the order 10 6 sm. As for the parameter (V 0i √ γ 0 )/ω p , it differs from the relativistic generalization of the Debye radius l D [14] (l D = (V T √ γ T )/ω p , where V T and γ T are the particle thermal velocity and Lorentz-factor respectively). On the other hand, it is selfevident that the following condition must be fulfilled:…”