Spatial characterization of a flare using radio observations and magnetic field topology

Using magnetograms, EUV and Hα images, Owens Valley Solar Array microwave observations, and 212-GHz flux density derived from the Solar Submillimeter Telescope data, we determine the spatial characteristics of the 1B/M6.9 flare that occurred on November 28, 2001, starting at 16:26 UT in active regio...

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Publicado:	2007
Materias:	Association with flares Dynamic spectrum Flares Magnetic reconnection Observational signatures Radio burst Relation to magnetic field Surges
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v240_n2_p271_Cristiani http://hdl.handle.net/20.500.12110/paper_00380938_v240_n2_p271_Cristiani
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_00380938_v240_n2_p271_Cristiani
record_format	dspace
spelling	paper:paper_00380938_v240_n2_p271_Cristiani2023-06-08T15:02:39Z Spatial characterization of a flare using radio observations and magnetic field topology Association with flares Dynamic spectrum Flares Magnetic reconnection Observational signatures Radio burst Relation to magnetic field Surges Using magnetograms, EUV and Hα images, Owens Valley Solar Array microwave observations, and 212-GHz flux density derived from the Solar Submillimeter Telescope data, we determine the spatial characteristics of the 1B/M6.9 flare that occurred on November 28, 2001, starting at 16:26 UT in active region (AR) NOAA 9715. This flare is associated with a chromospheric mass ejection or surge observed at 16:42 UT in the Hα images. We compute the coronal magnetic field under the linear force-free field assumption, constrained by the photospheric data of the Michelson Doppler Imager and loops observed by the Extreme Ultraviolet Imaging Telescope. The analysis of the magnetic field connectivity allows us to conclude that magnetic field reconnection between two different coronal/chromospheric sets of arches was at the origin of the flare and surge, respectively. The optically thick microwave spectrum at peak time shows a shape compatible with the emission from two different sites. Fitting gyrosynchrotron emission to the observed spectrum, we derive parameters for each source. © Springer 2007. 2007 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v240_n2_p271_Cristiani http://hdl.handle.net/20.500.12110/paper_00380938_v240_n2_p271_Cristiani
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	Association with flares Dynamic spectrum Flares Magnetic reconnection Observational signatures Radio burst Relation to magnetic field Surges
spellingShingle	Association with flares Dynamic spectrum Flares Magnetic reconnection Observational signatures Radio burst Relation to magnetic field Surges Spatial characterization of a flare using radio observations and magnetic field topology
topic_facet	Association with flares Dynamic spectrum Flares Magnetic reconnection Observational signatures Radio burst Relation to magnetic field Surges
description	Using magnetograms, EUV and Hα images, Owens Valley Solar Array microwave observations, and 212-GHz flux density derived from the Solar Submillimeter Telescope data, we determine the spatial characteristics of the 1B/M6.9 flare that occurred on November 28, 2001, starting at 16:26 UT in active region (AR) NOAA 9715. This flare is associated with a chromospheric mass ejection or surge observed at 16:42 UT in the Hα images. We compute the coronal magnetic field under the linear force-free field assumption, constrained by the photospheric data of the Michelson Doppler Imager and loops observed by the Extreme Ultraviolet Imaging Telescope. The analysis of the magnetic field connectivity allows us to conclude that magnetic field reconnection between two different coronal/chromospheric sets of arches was at the origin of the flare and surge, respectively. The optically thick microwave spectrum at peak time shows a shape compatible with the emission from two different sites. Fitting gyrosynchrotron emission to the observed spectrum, we derive parameters for each source. © Springer 2007.
title	Spatial characterization of a flare using radio observations and magnetic field topology
title_short	Spatial characterization of a flare using radio observations and magnetic field topology
title_full	Spatial characterization of a flare using radio observations and magnetic field topology
title_fullStr	Spatial characterization of a flare using radio observations and magnetic field topology
title_full_unstemmed	Spatial characterization of a flare using radio observations and magnetic field topology
title_sort	spatial characterization of a flare using radio observations and magnetic field topology
publishDate	2007
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v240_n2_p271_Cristiani http://hdl.handle.net/20.500.12110/paper_00380938_v240_n2_p271_Cristiani
_version_	1768545501514301440

Spatial characterization of a flare using radio observations and magnetic field topology

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