Filament interaction modeled by flux rope reconnection

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Hα observations of solar active region NOAA 10501 on 2003 November 20 revealed a very uncommon dynamic process: during the development of a nearby flare, two adjacent elongated filaments approached each other, merged at their middle sections, and separated again, thereby forming stable configuration...

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Autores principales:	Török, T., Chandra, R., Pariat, E., Démoulin, P., Schmieder, B., Aulanier, G., Linton, M.G., Mandrini, C.H.
Formato:	Artículo publishedVersion
Publicado:	2011
Materias:	Methods: numerical Sun: corona Sun: filaments, prominences
Acceso en línea:	http://hdl.handle.net/20.500.12110/paper_0004637X_v728_n1_p_Torok https://repositoriouba.sisbi.uba.ar/gsdl/cgi-bin/library.cgi?a=d&c=artiaex&d=paper_0004637X_v728_n1_p_Torok_oai
Aporte de:	Repositorio Digital de la Universidad de Buenos Aires (UBA) de Universidad de Buenos Aires

id	I28-R145-paper_0004637X_v728_n1_p_Torok_oai
record_format	dspace
spelling	I28-R145-paper_0004637X_v728_n1_p_Torok_oai2024-08-16 Török, T. Chandra, R. Pariat, E. Démoulin, P. Schmieder, B. Aulanier, G. Linton, M.G. Mandrini, C.H. 2011 Hα observations of solar active region NOAA 10501 on 2003 November 20 revealed a very uncommon dynamic process: during the development of a nearby flare, two adjacent elongated filaments approached each other, merged at their middle sections, and separated again, thereby forming stable configurations with new footpoint connections. The observed dynamic pattern is indicative of "slingshot" reconnection between two magnetic flux ropes. We test this scenario by means of a three-dimensional zero β magnetohydrodynamic simulation, using a modified version of the coronal flux rope model by Titov and Démoulin as the initial condition for the magnetic field. To this end, a configuration is constructed that contains two flux ropes which are oriented side-by-side and are embedded in an ambient potential field. The choice of the magnetic orientation of the flux ropes and of the topology of the potential field is guided by the observations. Quasi-static boundary flows are then imposed to bring the middle sections of the flux ropes into contact. After sufficient driving, the ropes reconnect and two new flux ropes are formed, which now connect the former adjacent flux rope footpoints of opposite polarity. The corresponding evolution of filament material is modeled by calculating the positions of field line dips at all times. The dips follow the morphological evolution of the flux ropes, in qualitative agreement with the observed filaments. © 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. Fil:Mandrini, C.H. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. application/pdf http://hdl.handle.net/20.500.12110/paper_0004637X_v728_n1_p_Torok info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar Astrophys. J. 2011;728(1) Methods: numerical Sun: corona Sun: filaments, prominences Filament interaction modeled by flux rope reconnection info:eu-repo/semantics/article info:ar-repo/semantics/artículo info:eu-repo/semantics/publishedVersion https://repositoriouba.sisbi.uba.ar/gsdl/cgi-bin/library.cgi?a=d&c=artiaex&d=paper_0004637X_v728_n1_p_Torok_oai
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-145
collection	Repositorio Digital de la Universidad de Buenos Aires (UBA)
topic	Methods: numerical Sun: corona Sun: filaments, prominences
spellingShingle	Methods: numerical Sun: corona Sun: filaments, prominences Török, T. Chandra, R. Pariat, E. Démoulin, P. Schmieder, B. Aulanier, G. Linton, M.G. Mandrini, C.H. Filament interaction modeled by flux rope reconnection
topic_facet	Methods: numerical Sun: corona Sun: filaments, prominences
description	Hα observations of solar active region NOAA 10501 on 2003 November 20 revealed a very uncommon dynamic process: during the development of a nearby flare, two adjacent elongated filaments approached each other, merged at their middle sections, and separated again, thereby forming stable configurations with new footpoint connections. The observed dynamic pattern is indicative of "slingshot" reconnection between two magnetic flux ropes. We test this scenario by means of a three-dimensional zero β magnetohydrodynamic simulation, using a modified version of the coronal flux rope model by Titov and Démoulin as the initial condition for the magnetic field. To this end, a configuration is constructed that contains two flux ropes which are oriented side-by-side and are embedded in an ambient potential field. The choice of the magnetic orientation of the flux ropes and of the topology of the potential field is guided by the observations. Quasi-static boundary flows are then imposed to bring the middle sections of the flux ropes into contact. After sufficient driving, the ropes reconnect and two new flux ropes are formed, which now connect the former adjacent flux rope footpoints of opposite polarity. The corresponding evolution of filament material is modeled by calculating the positions of field line dips at all times. The dips follow the morphological evolution of the flux ropes, in qualitative agreement with the observed filaments. © 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A.
format	Artículo Artículo publishedVersion
author	Török, T. Chandra, R. Pariat, E. Démoulin, P. Schmieder, B. Aulanier, G. Linton, M.G. Mandrini, C.H.
author_facet	Török, T. Chandra, R. Pariat, E. Démoulin, P. Schmieder, B. Aulanier, G. Linton, M.G. Mandrini, C.H.
author_sort	Török, T.
title	Filament interaction modeled by flux rope reconnection
title_short	Filament interaction modeled by flux rope reconnection
title_full	Filament interaction modeled by flux rope reconnection
title_fullStr	Filament interaction modeled by flux rope reconnection
title_full_unstemmed	Filament interaction modeled by flux rope reconnection
title_sort	filament interaction modeled by flux rope reconnection
publishDate	2011
url	http://hdl.handle.net/20.500.12110/paper_0004637X_v728_n1_p_Torok https://repositoriouba.sisbi.uba.ar/gsdl/cgi-bin/library.cgi?a=d&c=artiaex&d=paper_0004637X_v728_n1_p_Torok_oai
work_keys_str_mv	AT torokt filamentinteractionmodeledbyfluxropereconnection AT chandrar filamentinteractionmodeledbyfluxropereconnection AT pariate filamentinteractionmodeledbyfluxropereconnection AT demoulinp filamentinteractionmodeledbyfluxropereconnection AT schmiederb filamentinteractionmodeledbyfluxropereconnection AT aulanierg filamentinteractionmodeledbyfluxropereconnection AT lintonmg filamentinteractionmodeledbyfluxropereconnection AT mandrinich filamentinteractionmodeledbyfluxropereconnection
_version_	1809357049670139904

Filament interaction modeled by flux rope reconnection

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