Multi-resolution wavelet analysis of high time resolution millimeter wavelength observations of solar bursts

Autores
Giménez de Castro, C. G.; Raulin, J. P.; Mandrini, Cristina Hemilse; Kaufmann, Pierre; Magun, A.
Año de publicación
2001
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
By means of the wavelet representation of multi-resolution analysis, we study millimeter wavelength (mm-w) radio solar bursts obtained at 48 GHz with high time resolution (<=8 ms); observed at Itapetinga (Brazil). The multi-resolution analysis decomposes the signal locally both in time and in frequency, allowing us to identify the different temporal structures which underlie the flux density time series and the transient phenomena characteristic of solar bursts. The analysis was applied to the flux time profile of four solar bursts observed at a mm-w, studying separately the pre-flare, impulsive and post-flare phases when possible. We find that a wide range of time scales contributes to the radio flux. The minimum time scale found for the impulsive phase is 32 ms, after which the noise dominates the emission; the maximum is 8 s. Pre- and post-flare phases have a minimum time scale of 256 ms and a maximum between 1 to 8 s. Multi-resolution ``spectral indexes'', which are a measure of the self-similar behavior of the signal, are in some cases bigger for the impulsive phase than for the pre- and post-flare phases. We find that as the flux becomes higher the contribution from shorter time scales is enhanced.
Fil: Giménez de Castro, C. G.. Instituto Presbiteriano Mackenzie; Brasil
Fil: Raulin, J. P.. Instituto Presbiteriano Mackenzie; Brasil
Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Kaufmann, Pierre. Instituto Presbiteriano Mackenzie; Brasil
Fil: Magun, A.. University of Berne; Suiza
Materia
SOLAR FLARES
SOLAR RADIO RADIATION
SOLAR DATA ANALYSIS
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/22477
Acceder
id CONICETDig_d901a40b08ab142f38763abc17593f88
oai_identifier_str oai:ri.conicet.gov.ar:11336/22477
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Multi-resolution wavelet analysis of high time resolution millimeter wavelength observations of solar burstsGiménez de Castro, C. G.Raulin, J. P.Mandrini, Cristina HemilseKaufmann, PierreMagun, A.SOLAR FLARESSOLAR RADIO RADIATIONSOLAR DATA ANALYSIShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1By means of the wavelet representation of multi-resolution analysis, we study millimeter wavelength (mm-w) radio solar bursts obtained at 48 GHz with high time resolution (<=8 ms); observed at Itapetinga (Brazil). The multi-resolution analysis decomposes the signal locally both in time and in frequency, allowing us to identify the different temporal structures which underlie the flux density time series and the transient phenomena characteristic of solar bursts. The analysis was applied to the flux time profile of four solar bursts observed at a mm-w, studying separately the pre-flare, impulsive and post-flare phases when possible. We find that a wide range of time scales contributes to the radio flux. The minimum time scale found for the impulsive phase is 32 ms, after which the noise dominates the emission; the maximum is 8 s. Pre- and post-flare phases have a minimum time scale of 256 ms and a maximum between 1 to 8 s. Multi-resolution ``spectral indexes'', which are a measure of the self-similar behavior of the signal, are in some cases bigger for the impulsive phase than for the pre- and post-flare phases. We find that as the flux becomes higher the contribution from shorter time scales is enhanced.Fil: Giménez de Castro, C. G.. Instituto Presbiteriano Mackenzie; BrasilFil: Raulin, J. P.. Instituto Presbiteriano Mackenzie; BrasilFil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Kaufmann, Pierre. Instituto Presbiteriano Mackenzie; BrasilFil: Magun, A.. University of Berne; SuizaEDP Sciences2001-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/22477Giménez de Castro, C. G.; Raulin, J. P.; Mandrini, Cristina Hemilse; Kaufmann, Pierre; Magun, A.; Multi-resolution wavelet analysis of high time resolution millimeter wavelength observations of solar bursts; EDP Sciences; Astronomy and Astrophysics; 366; 1; 1-2001; 317-3250004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20000088info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2001/04/aa8452/aa8452.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:42:39Zoai:ri.conicet.gov.ar:11336/22477instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 10:42:39.782CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Multi-resolution wavelet analysis of high time resolution millimeter wavelength observations of solar bursts
title Multi-resolution wavelet analysis of high time resolution millimeter wavelength observations of solar bursts
spellingShingle Multi-resolution wavelet analysis of high time resolution millimeter wavelength observations of solar bursts
Giménez de Castro, C. G.
SOLAR FLARES
SOLAR RADIO RADIATION
SOLAR DATA ANALYSIS
title_short Multi-resolution wavelet analysis of high time resolution millimeter wavelength observations of solar bursts
title_full Multi-resolution wavelet analysis of high time resolution millimeter wavelength observations of solar bursts
title_fullStr Multi-resolution wavelet analysis of high time resolution millimeter wavelength observations of solar bursts
title_full_unstemmed Multi-resolution wavelet analysis of high time resolution millimeter wavelength observations of solar bursts
title_sort Multi-resolution wavelet analysis of high time resolution millimeter wavelength observations of solar bursts
dc.creator.none.fl_str_mv Giménez de Castro, C. G.
Raulin, J. P.
Mandrini, Cristina Hemilse
Kaufmann, Pierre
Magun, A.
author Giménez de Castro, C. G.
author_facet Giménez de Castro, C. G.
Raulin, J. P.
Mandrini, Cristina Hemilse
Kaufmann, Pierre
Magun, A.
author_role author
author2 Raulin, J. P.
Mandrini, Cristina Hemilse
Kaufmann, Pierre
Magun, A.
author2_role author
author
author
author
dc.subject.none.fl_str_mv SOLAR FLARES
SOLAR RADIO RADIATION
SOLAR DATA ANALYSIS
topic SOLAR FLARES
SOLAR RADIO RADIATION
SOLAR DATA ANALYSIS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv By means of the wavelet representation of multi-resolution analysis, we study millimeter wavelength (mm-w) radio solar bursts obtained at 48 GHz with high time resolution (<=8 ms); observed at Itapetinga (Brazil). The multi-resolution analysis decomposes the signal locally both in time and in frequency, allowing us to identify the different temporal structures which underlie the flux density time series and the transient phenomena characteristic of solar bursts. The analysis was applied to the flux time profile of four solar bursts observed at a mm-w, studying separately the pre-flare, impulsive and post-flare phases when possible. We find that a wide range of time scales contributes to the radio flux. The minimum time scale found for the impulsive phase is 32 ms, after which the noise dominates the emission; the maximum is 8 s. Pre- and post-flare phases have a minimum time scale of 256 ms and a maximum between 1 to 8 s. Multi-resolution ``spectral indexes'', which are a measure of the self-similar behavior of the signal, are in some cases bigger for the impulsive phase than for the pre- and post-flare phases. We find that as the flux becomes higher the contribution from shorter time scales is enhanced.
Fil: Giménez de Castro, C. G.. Instituto Presbiteriano Mackenzie; Brasil
Fil: Raulin, J. P.. Instituto Presbiteriano Mackenzie; Brasil
Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Kaufmann, Pierre. Instituto Presbiteriano Mackenzie; Brasil
Fil: Magun, A.. University of Berne; Suiza
description By means of the wavelet representation of multi-resolution analysis, we study millimeter wavelength (mm-w) radio solar bursts obtained at 48 GHz with high time resolution (<=8 ms); observed at Itapetinga (Brazil). The multi-resolution analysis decomposes the signal locally both in time and in frequency, allowing us to identify the different temporal structures which underlie the flux density time series and the transient phenomena characteristic of solar bursts. The analysis was applied to the flux time profile of four solar bursts observed at a mm-w, studying separately the pre-flare, impulsive and post-flare phases when possible. We find that a wide range of time scales contributes to the radio flux. The minimum time scale found for the impulsive phase is 32 ms, after which the noise dominates the emission; the maximum is 8 s. Pre- and post-flare phases have a minimum time scale of 256 ms and a maximum between 1 to 8 s. Multi-resolution ``spectral indexes'', which are a measure of the self-similar behavior of the signal, are in some cases bigger for the impulsive phase than for the pre- and post-flare phases. We find that as the flux becomes higher the contribution from shorter time scales is enhanced.
publishDate 2001
dc.date.none.fl_str_mv 2001-01
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/22477
Giménez de Castro, C. G.; Raulin, J. P.; Mandrini, Cristina Hemilse; Kaufmann, Pierre; Magun, A.; Multi-resolution wavelet analysis of high time resolution millimeter wavelength observations of solar bursts; EDP Sciences; Astronomy and Astrophysics; 366; 1; 1-2001; 317-325
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/22477
identifier_str_mv Giménez de Castro, C. G.; Raulin, J. P.; Mandrini, Cristina Hemilse; Kaufmann, Pierre; Magun, A.; Multi-resolution wavelet analysis of high time resolution millimeter wavelength observations of solar bursts; EDP Sciences; Astronomy and Astrophysics; 366; 1; 1-2001; 317-325
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20000088
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2001/04/aa8452/aa8452.html
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
_version_ 1844614459680620544
score 13.070432

Publicaciones similares