{"id":6906,"date":"2023-07-11T16:46:13","date_gmt":"2023-07-11T16:46:13","guid":{"rendered":"https:\/\/raege-az.pt\/?p=6906"},"modified":"2023-12-12T17:29:57","modified_gmt":"2023-12-12T17:29:57","slug":"c6-2-class-flare-parameters-inferred-with-a-3d-geometry-of-flare-database","status":"publish","type":"post","link":"https:\/\/raege-az.pt\/en\/c6-2-class-flare-parameters-inferred-with-a-3d-geometry-of-flare-database\/","title":{"rendered":"C6.2 class flare parameters inferred with a 3D geometry of flare database"},"content":{"rendered":"
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We analyzed a GOES C6.2 class flare on 27 October 2003 on the heliographic position S20E29. Based on the essential parameters of its microwave emission, we inferred a set of geometric and physical parameters to characterize a solar flare using a developed database of a simplified model of a 3D geometry of a magnetic loop. Based on the general properties of known solar flares and convoluted with the instrument resolution to replicate the observations from the Nobeyama radio polarimeter (NoRP) spectra and the Nobeyama radioheliograph (NoRH) brightness maps. Observed spectra and brightness distribution maps were compared with the modeled spectra and images in the database, indicating a possible range of unknown parameters. We computed a weighted mean of one hundred best model parameters ordered by increasing \u03c72<\/sup>. The solution was optimized as guess input to a final refinement with the Pikaia algorithm. We analyzed six different times, representing a flare\u2019s gradual, impulsive, and decay phases. We found at the time of burst maxima the energy spectral index \u223c5.74, photospheric magnetic field \u223c2543 G, non-thermal electron density \u223c109<\/sup> cm\u22121<\/sup>. We conclude that the physical parameters (magnetic field, energy spectral index, and non-thermal electron densities) are well recovered. However, the geometric parameters such as inclination, asymmetry, azimuth, loop radius, loop height, and foot separation are hard to fit due to a lack of instrument resolution of a precise geometry of a loop-like flare, eventually due to a loop-top emission or small-size loops that are not resolved.<\/p>\t\t\t\t\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t

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V. Cuambe[1]<\/sup>, J. Costa[2]<\/sup>, P. Sim\u00f5es[2]<\/sup><\/p>\t\t\t\t\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t

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Type\u00a0<\/strong>Presentation<\/p>

Event <\/strong>CESRA Workshop 2023<\/p>\t\t\t\t\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t

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[1] Esta\u00e7\u00e3o RAEGE de Santa Maria, Associa\u00e7\u00e3o RAEGE A\u00e7ores, Santa Maria – Azores, Portugal<\/p>\n

[2] Instituto de Pesquisas Espaciais, S\u00e3o Jos\u00e9 dos Campos-Brasil<\/p>\n

[3] Universidade Persbeteriana de Mackenzie, S\u00e3o Paulo – Brasil<\/p>\t\t\t\t\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t

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\n\t\t\t\t\t\n\t\t\t\t\t\t\n\t\t\t\t\t\t\t\t\tVoltar \u00e0 p\u00e1gina publica\u00e7\u00f5es<\/span>\n\t\t\t\t\t<\/span>\n\t\t\t\t\t<\/a>\n\t\t\t\t<\/div>\n\t\t\t\t\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/section>\n\t\t\t\t<\/div>","protected":false},"excerpt":{"rendered":"

We analyzed a GOES C6.2 class flare on 27 October 2003 on the heliographic position S20E29. Based on the essential parameters of its microwave emission, we inferred a set of geometric and physical parameters to characterize a solar flare using a developed database of a simplified model of a 3D geometry of a magnetic loop. […]<\/p>","protected":false},"author":1,"featured_media":0,"comment_status":"closed","ping_status":"closed","sticky":false,"template":"elementor_theme","format":"standard","meta":{"site-sidebar-layout":"default","site-content-layout":"default","ast-site-content-layout":"default","site-content-style":"default","site-sidebar-style":"default","ast-global-header-display":"","ast-banner-title-visibility":"","ast-main-header-display":"","ast-hfb-above-header-display":"","ast-hfb-below-header-display":"","ast-hfb-mobile-header-display":"","site-post-title":"","ast-breadcrumbs-content":"","ast-featured-img":"","footer-sml-layout":"","theme-transparent-header-meta":"default","adv-header-id-meta":"","stick-header-meta":"","header-above-stick-meta":"","header-main-stick-meta":"","header-below-stick-meta":"","astra-migrate-meta-layouts":"set","ast-page-background-enabled":"default","ast-page-background-meta":{"desktop":{"background-color":"","background-image":"","background-repeat":"repeat","background-position":"center center","background-size":"auto","background-attachment":"scroll","background-type":"","background-media":"","overlay-type":"","overlay-color":"","overlay-opacity":"","overlay-gradient":""},"tablet":{"background-color":"","background-image":"","background-repeat":"repeat","background-position":"center center","background-size":"auto","background-attachment":"scroll","background-type":"","background-media":"","overlay-type":"","overlay-color":"","overlay-opacity":"","overlay-gradient":""},"mobile":{"background-color":"","background-image":"","background-repeat":"repeat","background-position":"center center","background-size":"auto","background-attachment":"scroll","background-type":"","background-media":"","overlay-type":"","overlay-color":"","overlay-opacity":"","overlay-gradient":""}},"ast-content-background-meta":{"desktop":{"background-color":"var(--ast-global-color-5)","background-image":"","background-repeat":"repeat","background-position":"center center","background-size":"auto","background-attachment":"scroll","background-type":"","background-media":"","overlay-type":"","overlay-color":"","overlay-opacity":"","overlay-gradient":""},"tablet":{"background-color":"var(--ast-global-color-5)","background-image":"","background-repeat":"repeat","background-position":"center center","background-size":"auto","background-attachment":"scroll","background-type":"","background-media":"","overlay-type":"","overlay-color":"","overlay-opacity":"","overlay-gradient":""},"mobile":{"background-color":"var(--ast-global-color-5)","background-image":"","background-repeat":"repeat","background-position":"center center","background-size":"auto","background-attachment":"scroll","background-type":"","background-media":"","overlay-type":"","overlay-color":"","overlay-opacity":"","overlay-gradient":""}},"footnotes":""},"categories":[42,36,33],"tags":[],"class_list":["post-6906","post","type-post","status-publish","format-standard","hentry","category-42","category-apresentacao","category-publicacoes"],"yoast_head":"\nC6.2 class flare parameters inferred with a 3D geometry of flare database - RAEGE-Az<\/title>\n<meta name=\"robots\" content=\"index, follow, max-snippet:-1, max-image-preview:large, max-video-preview:-1\" \/>\n<link rel=\"canonical\" href=\"https:\/\/raege-az.pt\/en\/c6-2-class-flare-parameters-inferred-with-a-3d-geometry-of-flare-database\/\" \/>\n<meta property=\"og:locale\" content=\"en_GB\" \/>\n<meta property=\"og:type\" content=\"article\" \/>\n<meta property=\"og:title\" content=\"C6.2 class flare parameters inferred with a 3D geometry of flare database - RAEGE-Az\" \/>\n<meta property=\"og:description\" content=\"We analyzed a GOES C6.2 class flare on 27 October 2003 on the heliographic position S20E29. 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