Particle-in-cell and weak turbulence simulations of plasma emission
Autor(a) principal: | |
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Data de Publicação: | 2019 |
Outros Autores: | , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/196657 |
Resumo: | The plasma emission process, which is the mechanism for solar type II and type III radio burst phenomena, is studied by means of particle-in-cell (PIC) and weak turbulence (WT) simulation methods. “Plasma emission” is meant as a loose description of a series of processes, starting from the solar flare-associated electron beam exciting Langmuir and ion-acoustic turbulence, and subsequent partial conversion of beam energy into radiation energy by nonlinear processes. PIC simulation is rigorous but the method is computationally intense, and it is difficult to diagnose the results. The numerical solution of equations of WT theory, known as WT simulation, on the other hand, is efficient and naturally lends itself to diagnostics because various terms in the equation can be turned on or off. Nevertheless, WT theory is based upon a number of assumptions. It is therefore desirable to compare the two methods, which we do for the first time with numerical solutions of the complete set of equations of WT theory and a two-dimensional electromagnetic PIC simulation. Upon making quantitative comparisons, it is found that WT theory is largely valid, although some discrepancies are also found. The present study also indicates that large computational resources are required in order to accurately simulate the radiation emission processes, especially for low electron beam speeds, such that it may be more advantageous to employ the WT method in order to describe the radiation emission itself. Findings from the present paper thus imply that both methods may be useful for the study of solar radio emissions, as they are complementary. |
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Lee, Sang-YunZiebell, Luiz FernandoYoon, Peter H.Gaelzer, RudiLee, Ensang2019-07-09T02:38:18Z20190004-637Xhttp://hdl.handle.net/10183/196657001096264The plasma emission process, which is the mechanism for solar type II and type III radio burst phenomena, is studied by means of particle-in-cell (PIC) and weak turbulence (WT) simulation methods. “Plasma emission” is meant as a loose description of a series of processes, starting from the solar flare-associated electron beam exciting Langmuir and ion-acoustic turbulence, and subsequent partial conversion of beam energy into radiation energy by nonlinear processes. PIC simulation is rigorous but the method is computationally intense, and it is difficult to diagnose the results. The numerical solution of equations of WT theory, known as WT simulation, on the other hand, is efficient and naturally lends itself to diagnostics because various terms in the equation can be turned on or off. Nevertheless, WT theory is based upon a number of assumptions. It is therefore desirable to compare the two methods, which we do for the first time with numerical solutions of the complete set of equations of WT theory and a two-dimensional electromagnetic PIC simulation. Upon making quantitative comparisons, it is found that WT theory is largely valid, although some discrepancies are also found. The present study also indicates that large computational resources are required in order to accurately simulate the radiation emission processes, especially for low electron beam speeds, such that it may be more advantageous to employ the WT method in order to describe the radiation emission itself. Findings from the present paper thus imply that both methods may be useful for the study of solar radio emissions, as they are complementary.application/pdfengThe astrophysical journal. Bristol. Vol. 871, no. 1 (Jan. 2019), 74, 17 p.PlasmasMétodos analíticosTurbulênciaMétodos numéricosRadiação térmicaOndasMethods: analyticalMethods: numericalPlasmasRadiation processes: thermalTurbulenceWavesParticle-in-cell and weak turbulence simulations of plasma emissionEstrangeiroinfo:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFRGSinstname:Universidade Federal do Rio Grande do Sul (UFRGS)instacron:UFRGSTEXT001096264.pdf.txt001096264.pdf.txtExtracted Texttext/plain55567http://www.lume.ufrgs.br/bitstream/10183/196657/2/001096264.pdf.txt585168ecb03784ce8c8edad64f477518MD52ORIGINAL001096264.pdfTexto completo (inglês)application/pdf6176590http://www.lume.ufrgs.br/bitstream/10183/196657/1/001096264.pdfe096646203802cccca47dc47750e31c6MD5110183/1966572023-09-24 03:37:32.139518oai:www.lume.ufrgs.br:10183/196657Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2023-09-24T06:37:32Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Particle-in-cell and weak turbulence simulations of plasma emission |
title |
Particle-in-cell and weak turbulence simulations of plasma emission |
spellingShingle |
Particle-in-cell and weak turbulence simulations of plasma emission Lee, Sang-Yun Plasmas Métodos analíticos Turbulência Métodos numéricos Radiação térmica Ondas Methods: analytical Methods: numerical Plasmas Radiation processes: thermal Turbulence Waves |
title_short |
Particle-in-cell and weak turbulence simulations of plasma emission |
title_full |
Particle-in-cell and weak turbulence simulations of plasma emission |
title_fullStr |
Particle-in-cell and weak turbulence simulations of plasma emission |
title_full_unstemmed |
Particle-in-cell and weak turbulence simulations of plasma emission |
title_sort |
Particle-in-cell and weak turbulence simulations of plasma emission |
author |
Lee, Sang-Yun |
author_facet |
Lee, Sang-Yun Ziebell, Luiz Fernando Yoon, Peter H. Gaelzer, Rudi Lee, Ensang |
author_role |
author |
author2 |
Ziebell, Luiz Fernando Yoon, Peter H. Gaelzer, Rudi Lee, Ensang |
author2_role |
author author author author |
dc.contributor.author.fl_str_mv |
Lee, Sang-Yun Ziebell, Luiz Fernando Yoon, Peter H. Gaelzer, Rudi Lee, Ensang |
dc.subject.por.fl_str_mv |
Plasmas Métodos analíticos Turbulência Métodos numéricos Radiação térmica Ondas |
topic |
Plasmas Métodos analíticos Turbulência Métodos numéricos Radiação térmica Ondas Methods: analytical Methods: numerical Plasmas Radiation processes: thermal Turbulence Waves |
dc.subject.eng.fl_str_mv |
Methods: analytical Methods: numerical Plasmas Radiation processes: thermal Turbulence Waves |
description |
The plasma emission process, which is the mechanism for solar type II and type III radio burst phenomena, is studied by means of particle-in-cell (PIC) and weak turbulence (WT) simulation methods. “Plasma emission” is meant as a loose description of a series of processes, starting from the solar flare-associated electron beam exciting Langmuir and ion-acoustic turbulence, and subsequent partial conversion of beam energy into radiation energy by nonlinear processes. PIC simulation is rigorous but the method is computationally intense, and it is difficult to diagnose the results. The numerical solution of equations of WT theory, known as WT simulation, on the other hand, is efficient and naturally lends itself to diagnostics because various terms in the equation can be turned on or off. Nevertheless, WT theory is based upon a number of assumptions. It is therefore desirable to compare the two methods, which we do for the first time with numerical solutions of the complete set of equations of WT theory and a two-dimensional electromagnetic PIC simulation. Upon making quantitative comparisons, it is found that WT theory is largely valid, although some discrepancies are also found. The present study also indicates that large computational resources are required in order to accurately simulate the radiation emission processes, especially for low electron beam speeds, such that it may be more advantageous to employ the WT method in order to describe the radiation emission itself. Findings from the present paper thus imply that both methods may be useful for the study of solar radio emissions, as they are complementary. |
publishDate |
2019 |
dc.date.accessioned.fl_str_mv |
2019-07-09T02:38:18Z |
dc.date.issued.fl_str_mv |
2019 |
dc.type.driver.fl_str_mv |
Estrangeiro info:eu-repo/semantics/article |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
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publishedVersion |
dc.identifier.uri.fl_str_mv |
http://hdl.handle.net/10183/196657 |
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0004-637X |
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001096264 |
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http://hdl.handle.net/10183/196657 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
The astrophysical journal. Bristol. Vol. 871, no. 1 (Jan. 2019), 74, 17 p. |
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info:eu-repo/semantics/openAccess |
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openAccess |
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