On The Kinetic Stage Of Instability Of The Electron Beam - Solar Wind Plasma System

TL;DR

This paper analyzes the development of instability stages in electron beams within the solar wind plasma, highlighting the transition from hydrodynamic to kinetic instability and their effects on beam parameters and energy transfer.

Contribution

It provides a detailed theoretical analysis of the kinetic and hydrodynamic instability stages of electron beams in solar wind plasma, including parameter calculations and energy transfer insights.

Findings

Hydrodynamic instability lasts longer than homogeneous relaxation time.

Electron beam spreads up to 4 astronomical units during hydrodynamic stage.

More than half of the beam's kinetic energy is transferred to plasma oscillations.

Abstract

Within the framework of quasilinear theory it has been found that when radio bursts of III type are generated by the inhomogeneous system of electron beam - solar wind plasma, only time of development of the primary stage of instability, i.e., agnetohydrodynamic, is more than the total time of relaxation of an electron beam derived within the homogeneous model. During the development of hydrodynamic instability the electron beam is spread from the Sun to the distance of 4 astonomical unities. The hydrodynamic stage is followed by the development of kinetic instability leading, ultimately, to the formation of horizontal plateau in the beam region at the tail of Maxwell distribution. Parameters of the plateau, such as its length and height, have been calculated as characteristic parameters of an electron beam generated by the active solar bursts. In the development of kinetic beam instability more than a half of kinetic energy of the beam is transmitted to plasma oscillations.