Homologous Flares and Magnetic Field Topology in Active Region NOAA 10501 on 20 November 2003

We present and interpret observations of two morphologically homologous flares that occurred in active region (AR) NOAA 10501 on 20 November 2003. Both flares displayed four homologous Hα ribbons and were both accompanied by coronal mass ejections (CMEs). The central flare ribbons were located at th...

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Detalles Bibliográficos
Publicado: 2011
Materias:
Active regions, magnetic fields
Flares, dynamics
Flares, relation to magnetic field
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v269_n1_p83_Chandra
http://hdl.handle.net/20.500.12110/paper_00380938_v269_n1_p83_Chandra
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_00380938_v269_n1_p83_Chandra
record_format dspace
spelling paper:paper_00380938_v269_n1_p83_Chandra2023-06-08T15:02:45Z Homologous Flares and Magnetic Field Topology in Active Region NOAA 10501 on 20 November 2003 Active regions, magnetic fields Flares, dynamics Flares, relation to magnetic field We present and interpret observations of two morphologically homologous flares that occurred in active region (AR) NOAA 10501 on 20 November 2003. Both flares displayed four homologous Hα ribbons and were both accompanied by coronal mass ejections (CMEs). The central flare ribbons were located at the site of an emerging bipole in the centre of the active region. The negative polarity of this bipole fragmented in two main pieces, one rotating around the positive polarity by ≈ 110° within 32 hours. We model the coronal magnetic field and compute its topology, using as boundary condition the magnetogram closest in time to each flare. In particular, we calculate the location of quasi-separatrix layers (QSLs) in order to understand the connectivity between the flare ribbons. Though several polarities were present in AR 10501, the global magnetic field topology corresponds to a quadrupolar magnetic field distribution without magnetic null points. For both flares, the photospheric traces of QSLs are similar and match well the locations of the four Hα ribbons. This globally unchanged topology and the continuous shearing by the rotating bipole are two key factors responsible for the flare homology. However, our analyses also indicate that different magnetic connectivity domains of the quadrupolar configuration become unstable during each flare, so that magnetic reconnection proceeds differently in both events. © 2010 Springer Science+Business Media B.V. 2011 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v269_n1_p83_Chandra http://hdl.handle.net/20.500.12110/paper_00380938_v269_n1_p83_Chandra
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Active regions, magnetic fields
Flares, dynamics
Flares, relation to magnetic field
spellingShingle Active regions, magnetic fields
Flares, dynamics
Flares, relation to magnetic field
Homologous Flares and Magnetic Field Topology in Active Region NOAA 10501 on 20 November 2003
topic_facet Active regions, magnetic fields
Flares, dynamics
Flares, relation to magnetic field
description We present and interpret observations of two morphologically homologous flares that occurred in active region (AR) NOAA 10501 on 20 November 2003. Both flares displayed four homologous Hα ribbons and were both accompanied by coronal mass ejections (CMEs). The central flare ribbons were located at the site of an emerging bipole in the centre of the active region. The negative polarity of this bipole fragmented in two main pieces, one rotating around the positive polarity by ≈ 110° within 32 hours. We model the coronal magnetic field and compute its topology, using as boundary condition the magnetogram closest in time to each flare. In particular, we calculate the location of quasi-separatrix layers (QSLs) in order to understand the connectivity between the flare ribbons. Though several polarities were present in AR 10501, the global magnetic field topology corresponds to a quadrupolar magnetic field distribution without magnetic null points. For both flares, the photospheric traces of QSLs are similar and match well the locations of the four Hα ribbons. This globally unchanged topology and the continuous shearing by the rotating bipole are two key factors responsible for the flare homology. However, our analyses also indicate that different magnetic connectivity domains of the quadrupolar configuration become unstable during each flare, so that magnetic reconnection proceeds differently in both events. © 2010 Springer Science+Business Media B.V.
title Homologous Flares and Magnetic Field Topology in Active Region NOAA 10501 on 20 November 2003
title_short Homologous Flares and Magnetic Field Topology in Active Region NOAA 10501 on 20 November 2003
title_full Homologous Flares and Magnetic Field Topology in Active Region NOAA 10501 on 20 November 2003
title_fullStr Homologous Flares and Magnetic Field Topology in Active Region NOAA 10501 on 20 November 2003
title_full_unstemmed Homologous Flares and Magnetic Field Topology in Active Region NOAA 10501 on 20 November 2003
title_sort homologous flares and magnetic field topology in active region noaa 10501 on 20 november 2003
publishDate 2011
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v269_n1_p83_Chandra
http://hdl.handle.net/20.500.12110/paper_00380938_v269_n1_p83_Chandra
_version_ 1768544948323352576

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