Development Of Two-stream Instability Research Articles

Two-stream instability generation in the lunar ionosphere

The Two-stream Instability (TSI) generation is studied analytically in the lunar ionosphere. The TSI is a tiny perturbation in the electron plasma density, due to which an electric field grows with time and this growth is facilitated by the electron plasma in the background. In lunar ionosphere, the TSI comes into existence when the solar wind interacts unhindered with the tenuous lunar electron plasma in the surface bound exosphere. In this study, the conditions which allow the TSI to form and the subsequent instability growth with time i.e. the growth factor, is estimated. Initially, the threshold condition for the TSI to take place is determined. Thereafter, the solar wind and lunar plasma parameter contribution to trigger TSI is investigated along with the effect of these parameters in the evolution of TSI. The plasma TSI evolution with the passage of time is also depicted in phase space diagram with Particle-In-Cell simulations.

Density Profile of a Plasma Layer Formed by an Electron Beam

Results of particle-in-cell simulation of the formation of a near-wall plasma layer produced by an ionization source remote from the chamber walls are verified experimentally. The measured profiles of the density and temperature of the plasma produced by an electron beam in two modes are compared: (i) gas is ionized by a low-density electron beam, while collective interactions are almost absent (beam-induced plasma), and (ii) gas is mainly ionized by plasma electrons heated due to the development of two-stream instability (beam−plasma discharge). The measured spatial profiles of the parameters of the beam-induced plasma are found to qualitatively agree with the model ones.

Plural interactions of space charge wave harmonics during the development of two-stream instability

We construct a cubically nonlinear theory of plural interactions between harmonics of the growing space charge wave (SCW) during the development of the two-stream instability. It is shown that the SCW with a wide frequency spectrum is formed when the frequency of the first SCW harmonic is much lower than the critical frequency of the two-stream instability. Such SCW has part of the spectrum in which higher harmonics have higher amplitudes. We analyze the dynamics of the plural harmonic interactions of the growing SCW and define the saturation harmonic levels. We find the mechanisms of forming the multiharmonic SCW for the waves with frequencies lower than the critical frequency and for the waves with frequencies that exceed the critical frequency.

Effect of parametric resonance on the formation of waves with a broad multiharmonic spectrum during the development of two-stream instability

A cubically nonlinear multiharmonic theory of two-stream instability in a two-velocity relativistic electron beam is constructed with allowance for parametric resonance between harmonics of longitudinal waves of different types, as well as between wave harmonics of the same type. The effect of these two kinds of parametric resonance interaction on the development of two-stream instability is investigated. It is shown that parametric resonance between different types of longitudinal waves excited in a two-velocity beam can substantially affect the development of physical processes in the system under study. It is proposed to use parametric resonance between longitudinal waves of different types to form waves with a prescribed broad multiharmonic spectrum.

Characteristic features of the development of two-stream instability of electron beams in the presence of spatially localized perturbations

A study is made of the evolution of a spatially localized perturbation in the form of a Gaussian packet during two-stream instability in a plasma. It is shown that, on the whole, the moving perturbation is decelerated and its shape is distorted; moreover, the higher the group velocity of the packet, the higher the deceleration rate.

About the Magnetic Field Generation in Crab Nebula

AbstractThe new plasma mechanism for the magnetic field generation in Crab Nebula is suggested. The mechanism is based on the development of two-stream instability after the supernova explosion.

Two-stream instability in a collisionless plasma

This paper discusses the development of two-stream instability in a collisionless plasma. The plasma is described by velocity moments of Vlasov equation where heat flow tensor has been neglected. A dispersion relation for arbitrary propagation is derived for a collisionless electron fluid. Special cases of propagation parallel and perpendicular to the field lines are discussed. Growth rate is computed for parameters representative of the shear layers of solar wind at one AU. It is found that the shear layers are likely to be overstable.