Nonlinear stability of solar type III radio bursts. I. Theory.
Abstract
A theory of the excitation of solar type III bursts is presented. Electrons initially unstable to the linear bumpintail instability are shown to rapidly amplify Langmuir waves to energy densities characteristic of strong turbulence. The threedimensional equations which describe the strong coupling (wavewave) interactions are derived. For parameters characteristic of the interplanetary medium the equations reduce to onedimension. In that case the oscillating twostream instability (OTSI) is the dominant nonlinear instability. OTSI is stabilized through the production of nonlinear ion density fluctuations that efficiently scatter Langmuir waves out of resonance with the electron beam. An analytical model of the electron distribution function is also developed which is used to estimate the total energy losses suffered by the electron beam as it propagates from the solar corona to 1 AU and beyond.
 Publication:

The Astrophysical Journal
 Pub Date:
 November 1979
 DOI:
 10.1086/157502
 Bibcode:
 1979ApJ...234..348S
 Keywords:

 Magnetohydrodynamic Stability;
 Solar Physics;
 Type 3 Bursts;
 Coupling Coefficients;
 Density Distribution;
 Electron Flux Density;
 Electron Oscillations;
 Energy Dissipation;
 Interplanetary Medium;
 Ion Density (Concentration);
 Nonlinearity;
 Numerical Analysis;
 Wave Interaction;
 Solar Physics;
 Magnetohydrodynamics:Solar Radio Bursts