Analysis of Intermittency in Submillimeter Radio and Hard X-Ray Data During the Impulsive Phase of a Solar Flare

We present an analysis of intermittent processes occurring during the impulsive phase of the flare SOL2012-03-13, using hard X-rays and submillimeter radio data. Intermittency is a key characteristic in turbulent plasmas and has so far only been analyzed for hard X-ray data. Since in a typical flare...

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Autores principales:	Giménez de Castro, G., Simões, P.J.A., Raulin, J.-P., Guimarães, O.M., Jr.
Formato:	JOUR
Materias:	Avalanche models Hard X-rays, Solar flares Intermittency Microwave, Solar flares Wavelets
Acceso en línea:	http://hdl.handle.net/20.500.12110/paper_00380938_v291_n7_p2003_GimenezdeCastro
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	todo:paper_00380938_v291_n7_p2003_GimenezdeCastro
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spelling	todo:paper_00380938_v291_n7_p2003_GimenezdeCastro2023-10-03T14:48:55Z Analysis of Intermittency in Submillimeter Radio and Hard X-Ray Data During the Impulsive Phase of a Solar Flare Giménez de Castro, G. Simões, P.J.A. Raulin, J.-P. Guimarães, O.M., Jr. Avalanche models Hard X-rays, Solar flares Intermittency Microwave, Solar flares Wavelets We present an analysis of intermittent processes occurring during the impulsive phase of the flare SOL2012-03-13, using hard X-rays and submillimeter radio data. Intermittency is a key characteristic in turbulent plasmas and has so far only been analyzed for hard X-ray data. Since in a typical flare the same accelerated electron population is believed to produce both hard X-rays and gyrosynchrotron radiation, we compare the two time profiles by searching for intermittency signatures. For this, we define a cross-wavelet power spectrum, which is used to obtain the local intermittency measure, or LIM. When greater than three, the square LIM coefficients indicate a local intermittent process. The LIM2 coefficient distribution in time and scale helps to identify avalanche or cascade energy release processes. We find two different and well-separated intermittent behaviors in the submillimeter data: for scales greater than 20 s, a broad distribution during the rising and maximum phases of the emission seems to favor a cascade process; for scales below 1 s, short pulses centered on the peak time are representative of avalanches. When applying the same analysis to hard X-rays, we find that only the scales above 10 s produce a distribution related to a cascade energy fragmentation. Our results suggest that different acceleration mechanisms are responsible for tens of keV and MeV energy ranges of electrons. © 2016, Springer Science+Business Media Dordrecht. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00380938_v291_n7_p2003_GimenezdeCastro
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	Avalanche models Hard X-rays, Solar flares Intermittency Microwave, Solar flares Wavelets
spellingShingle	Avalanche models Hard X-rays, Solar flares Intermittency Microwave, Solar flares Wavelets Giménez de Castro, G. Simões, P.J.A. Raulin, J.-P. Guimarães, O.M., Jr. Analysis of Intermittency in Submillimeter Radio and Hard X-Ray Data During the Impulsive Phase of a Solar Flare
topic_facet	Avalanche models Hard X-rays, Solar flares Intermittency Microwave, Solar flares Wavelets
description	We present an analysis of intermittent processes occurring during the impulsive phase of the flare SOL2012-03-13, using hard X-rays and submillimeter radio data. Intermittency is a key characteristic in turbulent plasmas and has so far only been analyzed for hard X-ray data. Since in a typical flare the same accelerated electron population is believed to produce both hard X-rays and gyrosynchrotron radiation, we compare the two time profiles by searching for intermittency signatures. For this, we define a cross-wavelet power spectrum, which is used to obtain the local intermittency measure, or LIM. When greater than three, the square LIM coefficients indicate a local intermittent process. The LIM2 coefficient distribution in time and scale helps to identify avalanche or cascade energy release processes. We find two different and well-separated intermittent behaviors in the submillimeter data: for scales greater than 20 s, a broad distribution during the rising and maximum phases of the emission seems to favor a cascade process; for scales below 1 s, short pulses centered on the peak time are representative of avalanches. When applying the same analysis to hard X-rays, we find that only the scales above 10 s produce a distribution related to a cascade energy fragmentation. Our results suggest that different acceleration mechanisms are responsible for tens of keV and MeV energy ranges of electrons. © 2016, Springer Science+Business Media Dordrecht.
format	JOUR
author	Giménez de Castro, G. Simões, P.J.A. Raulin, J.-P. Guimarães, O.M., Jr.
author_facet	Giménez de Castro, G. Simões, P.J.A. Raulin, J.-P. Guimarães, O.M., Jr.
author_sort	Giménez de Castro, G.
title	Analysis of Intermittency in Submillimeter Radio and Hard X-Ray Data During the Impulsive Phase of a Solar Flare
title_short	Analysis of Intermittency in Submillimeter Radio and Hard X-Ray Data During the Impulsive Phase of a Solar Flare
title_full	Analysis of Intermittency in Submillimeter Radio and Hard X-Ray Data During the Impulsive Phase of a Solar Flare
title_fullStr	Analysis of Intermittency in Submillimeter Radio and Hard X-Ray Data During the Impulsive Phase of a Solar Flare
title_full_unstemmed	Analysis of Intermittency in Submillimeter Radio and Hard X-Ray Data During the Impulsive Phase of a Solar Flare
title_sort	analysis of intermittency in submillimeter radio and hard x-ray data during the impulsive phase of a solar flare
url	http://hdl.handle.net/20.500.12110/paper_00380938_v291_n7_p2003_GimenezdeCastro
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Analysis of Intermittency in Submillimeter Radio and Hard X-Ray Data During the Impulsive Phase of a Solar Flare

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