Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (62) (Citation History)
· Refereed Citations to the Article
· Reads History
·
· Translate This Page
Title:
Nonlinear stability of solar type III radio bursts. I - Theory
Authors:
Smith, R. A.; Goldstein, M. L.; Papadopoulos, K.
Affiliation:
AA(Paris, Observatoire, Meudon, Hauts-de-Seine, France), AB(NASA, Goddard Space Flight Center, Laboratory for Extraterrestrial Physics, Greenbelt, Md.), AC(U.S. Navy, Naval Research Laboratory, Washington, D.C.)
Publication:
Astrophysical Journal, Part 1, vol. 234, Nov. 15, 1979, p. 348-362. Navy-supported research. (ApJ Homepage)
Publication Date:
11/1979
Category:
Solar Physics
Origin:
STI
NASA/STI 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
DOI:
10.1086/157502
Bibliographic Code:
1979ApJ...234..348S

Abstract

A theory of the excitation of solar type III bursts is presented. Electrons initially unstable to the linear bump-in-tail instability are shown to rapidly amplify Langmuir waves to energy densities characteristic of strong turbulence. The three-dimensional equations which describe the strong coupling (wave-wave) interactions are derived. For parameters characteristic of the interplanetary medium the equations reduce to one-dimension. In that case the oscillating two-stream 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.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences



More Article Retrieval Options

HELP for Article Retrieval


Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

  New!

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints