Use of RHESSI observations to determine the origin and fate of non-thermal flare electrons

Most analyses of the characteristics of hard X-ray emission from solar flares have relied on observations of the spectral, temporal and spatial intensity distribution obtained by different instruments and, in the majority of cases, different events. The Reuven Ramaty High Energy Spectroscopic Imager...

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Guardado en:
Detalles Bibliográficos
Publicado: 2004
Materias:
Hard X-rays
Particle acceleration
Solar flares
Electron emission
Image processing
Spectroscopic analysis
X rays
Electron energization
Flare loops
Thermalization
X-ray emission
Space research
solar activity
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_02731177_v34_n2_p451_Machado
http://hdl.handle.net/20.500.12110/paper_02731177_v34_n2_p451_Machado
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_02731177_v34_n2_p451_Machado
record_format dspace
spelling paper:paper_02731177_v34_n2_p451_Machado2025-07-30T18:03:26Z Use of RHESSI observations to determine the origin and fate of non-thermal flare electrons Hard X-rays Particle acceleration Solar flares Electron emission Image processing Spectroscopic analysis X rays Electron energization Flare loops Thermalization X-ray emission Space research solar activity Most analyses of the characteristics of hard X-ray emission from solar flares have relied on observations of the spectral, temporal and spatial intensity distribution obtained by different instruments and, in the majority of cases, different events. The Reuven Ramaty High Energy Spectroscopic Imager gives us the possibility of combining all three fundamental parameters in a single set of observations from the same instrument. In this paper, we describe a method to compute the distribution of hard X-ray emission in flare loops, which can be used to determine the characteristics of electron energization, transport and thermalization during short lived impulsive peaks. © 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. 2004 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_02731177_v34_n2_p451_Machado http://hdl.handle.net/20.500.12110/paper_02731177_v34_n2_p451_Machado
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Hard X-rays
Particle acceleration
Solar flares
Electron emission
Image processing
Spectroscopic analysis
X rays
Electron energization
Flare loops
Thermalization
X-ray emission
Space research
solar activity
spellingShingle Hard X-rays
Particle acceleration
Solar flares
Electron emission
Image processing
Spectroscopic analysis
X rays
Electron energization
Flare loops
Thermalization
X-ray emission
Space research
solar activity
Use of RHESSI observations to determine the origin and fate of non-thermal flare electrons
topic_facet Hard X-rays
Particle acceleration
Solar flares
Electron emission
Image processing
Spectroscopic analysis
X rays
Electron energization
Flare loops
Thermalization
X-ray emission
Space research
solar activity
description Most analyses of the characteristics of hard X-ray emission from solar flares have relied on observations of the spectral, temporal and spatial intensity distribution obtained by different instruments and, in the majority of cases, different events. The Reuven Ramaty High Energy Spectroscopic Imager gives us the possibility of combining all three fundamental parameters in a single set of observations from the same instrument. In this paper, we describe a method to compute the distribution of hard X-ray emission in flare loops, which can be used to determine the characteristics of electron energization, transport and thermalization during short lived impulsive peaks. © 2004 COSPAR. Published by Elsevier Ltd. All rights reserved.
title Use of RHESSI observations to determine the origin and fate of non-thermal flare electrons
title_short Use of RHESSI observations to determine the origin and fate of non-thermal flare electrons
title_full Use of RHESSI observations to determine the origin and fate of non-thermal flare electrons
title_fullStr Use of RHESSI observations to determine the origin and fate of non-thermal flare electrons
title_full_unstemmed Use of RHESSI observations to determine the origin and fate of non-thermal flare electrons
title_sort use of rhessi observations to determine the origin and fate of non-thermal flare electrons
publishDate 2004
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_02731177_v34_n2_p451_Machado
http://hdl.handle.net/20.500.12110/paper_02731177_v34_n2_p451_Machado
_version_ 1840323718894583808

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