Beam-generated plasma turbulence during solar flares

We develop a simple theoretical model to analyze the harmonic plasma radiation produced by an electron beam injected in a flaring loop and traveling along its magnetic field lines. For a given atmospheric model, we consistently consider collisional effects and the generation of Langmuir waves as a f...

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Autores principales:	Vasquez, A.M., Gomez, D.O.
Formato:	JOUR
Materias:	Sun: flares Sun: radio radiation Turbulence Waves
Acceso en línea:	http://hdl.handle.net/20.500.12110/paper_0004637X_v484_n1PARTI_p463_Vasquez
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	todo:paper_0004637X_v484_n1PARTI_p463_Vasquez
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spelling	todo:paper_0004637X_v484_n1PARTI_p463_Vasquez2023-10-03T14:01:42Z Beam-generated plasma turbulence during solar flares Vasquez, A.M. Gomez, D.O. Sun: flares Sun: radio radiation Turbulence Waves We develop a simple theoretical model to analyze the harmonic plasma radiation produced by an electron beam injected in a flaring loop and traveling along its magnetic field lines. For a given atmospheric model, we consistently consider collisional effects and the generation of Langmuir waves as a function of the atmospheric depth. Langmuir wave generation is assumed to saturate by quasilinear relaxation, which in turn causes the electron distribution function to develop a plateau at its low-energy end. We formulate an iterative procedure to integrate the coupled equations for the electron distribution function and the wave energy density, taking advantage of the fact that quasilinear relaxation occurs on times much shorter than the collisional timescale. From the wave energy density as a function of depth, we computed the microwave flux generated by second harmonic radiation, taking into account the optical thickness due to the reverse process. Previous studies yield microwave fluxes much larger than those derived from observations. The smaller levels of turbulence obtained from this model, and the lower emissivity due to the relaxation of the head-on approximation, contribute to reduce significantly the predicted microwave emission. We suggest that the simplicity of the present model makes it suitable for the quantitative analysis of spatially resolved radio observations in the GHz range. © 1997. The American Astronomical Socieiy. All rights reserved. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_0004637X_v484_n1PARTI_p463_Vasquez
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	Sun: flares Sun: radio radiation Turbulence Waves
spellingShingle	Sun: flares Sun: radio radiation Turbulence Waves Vasquez, A.M. Gomez, D.O. Beam-generated plasma turbulence during solar flares
topic_facet	Sun: flares Sun: radio radiation Turbulence Waves
description	We develop a simple theoretical model to analyze the harmonic plasma radiation produced by an electron beam injected in a flaring loop and traveling along its magnetic field lines. For a given atmospheric model, we consistently consider collisional effects and the generation of Langmuir waves as a function of the atmospheric depth. Langmuir wave generation is assumed to saturate by quasilinear relaxation, which in turn causes the electron distribution function to develop a plateau at its low-energy end. We formulate an iterative procedure to integrate the coupled equations for the electron distribution function and the wave energy density, taking advantage of the fact that quasilinear relaxation occurs on times much shorter than the collisional timescale. From the wave energy density as a function of depth, we computed the microwave flux generated by second harmonic radiation, taking into account the optical thickness due to the reverse process. Previous studies yield microwave fluxes much larger than those derived from observations. The smaller levels of turbulence obtained from this model, and the lower emissivity due to the relaxation of the head-on approximation, contribute to reduce significantly the predicted microwave emission. We suggest that the simplicity of the present model makes it suitable for the quantitative analysis of spatially resolved radio observations in the GHz range. © 1997. The American Astronomical Socieiy. All rights reserved.
format	JOUR
author	Vasquez, A.M. Gomez, D.O.
author_facet	Vasquez, A.M. Gomez, D.O.
author_sort	Vasquez, A.M.
title	Beam-generated plasma turbulence during solar flares
title_short	Beam-generated plasma turbulence during solar flares
title_full	Beam-generated plasma turbulence during solar flares
title_fullStr	Beam-generated plasma turbulence during solar flares
title_full_unstemmed	Beam-generated plasma turbulence during solar flares
title_sort	beam-generated plasma turbulence during solar flares
url	http://hdl.handle.net/20.500.12110/paper_0004637X_v484_n1PARTI_p463_Vasquez
work_keys_str_mv	AT vasquezam beamgeneratedplasmaturbulenceduringsolarflares AT gomezdo beamgeneratedplasmaturbulenceduringsolarflares
_version_	1807322507208818688

Beam-generated plasma turbulence during solar flares

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