Plasma emission by nonlinear electromagnetic processes

• Autor(a) principal: Ziebell, Luiz Fernando
• Data de Publicação: 2015
• Outros Autores: Yoon, Peter H., Petruzzellis, Larissa Teixeira, Gaelzer, Rudi, Pavan, Joel
• Tipo de documento: Artigo
• Idioma: eng
• Título da fonte: Repositório Institucional da UFRGS
• Texto Completo: http://hdl.handle.net/10183/126986
• topic: Plasmas astrofisicos; Instabilidade em plasmas; Ondas de Langmuir em plasmas; Vento solar; Mecanismos de radiação em astrofísica; Radiação solar em radio-frequência; Plasmas; Radiation mechanisms: non-thermal; Solar wind; Sun: radio radiation; Turbulence; Waves

The plasma emission, or electromagnetic (EM) radiation at the plasma frequency and/or its harmonic(s), is generally accepted as the radiation mechanism responsible for solar type II and III radio bursts. Identification and characterization of these solar radio burst phenomena were done in the 1950s. Despite many decades of theoretical research since then, a rigorous demonstration of the plasma emission process based upon first principles was not available until recently, when, in a recent Letter, Ziebell et al. reported the first complete numerical solution of EM weak turbulence equations; thus, quantitatively analyzing the plasma emission process starting from the initial electron beam and the associated beam-plasma (or Langmuir wave) instability, as well as the subsequent nonlinear conversion of electrostatic Langmuir turbulence into EM radiation. In the present paper, the same problem is revisited in order to elucidate the detailed physical mechanisms that could not be reported in the brief Letter format. Findings from the present paper may be useful for interpreting observations and full-particle numerical simulations.