Properties of fast submillimeter time structures during a large solar flare

We report properties of fast varying submillimeter emission during one of the strongest solar radio flares of solar cycle 23. Emission was obtained by the Solar Submillimeter-Wave Telescope at 212 and 405 GHz and compared with hard X-ray and γ-ray counts up to few tens of MeV photon energy ranges. W...

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Guardado en:
Detalles Bibliográficos
Publicado: 2003
Materias:
Gamma rays: bursts
Sun: flares
Sun: radio radiation
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v592_n1I_p580_Raulin
http://hdl.handle.net/20.500.12110/paper_0004637X_v592_n1I_p580_Raulin
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_0004637X_v592_n1I_p580_Raulin
record_format dspace
spelling paper:paper_0004637X_v592_n1I_p580_Raulin2023-06-08T14:28:48Z Properties of fast submillimeter time structures during a large solar flare Gamma rays: bursts Sun: flares Sun: radio radiation We report properties of fast varying submillimeter emission during one of the strongest solar radio flares of solar cycle 23. Emission was obtained by the Solar Submillimeter-Wave Telescope at 212 and 405 GHz and compared with hard X-ray and γ-ray counts up to few tens of MeV photon energy ranges. We employ different methods to detect and characterize flux density variations and find that during the impulsive phase of the event, the closer in time to the peak flare, the higher the occurrence of the fastest and brightest time structures. The good comparison with hard X-ray and γ-ray count rates indicates that fast submillimeter pulses are the signatures of primary energetic injections. The characteristics of the fast spikes at 212 and 405 GHz, such as their flux density and localization, compared to those of the underlying slower impulsive component, also suggest that their nature is different. 2003 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v592_n1I_p580_Raulin http://hdl.handle.net/20.500.12110/paper_0004637X_v592_n1I_p580_Raulin
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Gamma rays: bursts
Sun: flares
Sun: radio radiation
spellingShingle Gamma rays: bursts
Sun: flares
Sun: radio radiation
Properties of fast submillimeter time structures during a large solar flare
topic_facet Gamma rays: bursts
Sun: flares
Sun: radio radiation
description We report properties of fast varying submillimeter emission during one of the strongest solar radio flares of solar cycle 23. Emission was obtained by the Solar Submillimeter-Wave Telescope at 212 and 405 GHz and compared with hard X-ray and γ-ray counts up to few tens of MeV photon energy ranges. We employ different methods to detect and characterize flux density variations and find that during the impulsive phase of the event, the closer in time to the peak flare, the higher the occurrence of the fastest and brightest time structures. The good comparison with hard X-ray and γ-ray count rates indicates that fast submillimeter pulses are the signatures of primary energetic injections. The characteristics of the fast spikes at 212 and 405 GHz, such as their flux density and localization, compared to those of the underlying slower impulsive component, also suggest that their nature is different.
title Properties of fast submillimeter time structures during a large solar flare
title_short Properties of fast submillimeter time structures during a large solar flare
title_full Properties of fast submillimeter time structures during a large solar flare
title_fullStr Properties of fast submillimeter time structures during a large solar flare
title_full_unstemmed Properties of fast submillimeter time structures during a large solar flare
title_sort properties of fast submillimeter time structures during a large solar flare
publishDate 2003
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v592_n1I_p580_Raulin
http://hdl.handle.net/20.500.12110/paper_0004637X_v592_n1I_p580_Raulin
_version_ 1768542295299194880

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