Filament interaction modeled by flux rope reconnection

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...

Descripción completa

Guardado en:

Detalles Bibliográficos
Autor principal:	Mandrini, Cristina Hemilse
Publicado:	2011
Materias:	Methods: numerical Sun: corona Sun: filaments, prominences
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v728_n1_p_Torok http://hdl.handle.net/20.500.12110/paper_0004637X_v728_n1_p_Torok
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_0004637X_v728_n1_p_Torok
record_format	dspace
spelling	paper:paper_0004637X_v728_n1_p_Torok2023-06-08T14:29:01Z Filament interaction modeled by flux rope reconnection Mandrini, Cristina Hemilse Methods: numerical Sun: corona Sun: filaments, prominences 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. 2011 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v728_n1_p_Torok http://hdl.handle.net/20.500.12110/paper_0004637X_v728_n1_p_Torok
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	Methods: numerical Sun: corona Sun: filaments, prominences
spellingShingle	Methods: numerical Sun: corona Sun: filaments, prominences Mandrini, Cristina Hemilse 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.
author	Mandrini, Cristina Hemilse
author_facet	Mandrini, Cristina Hemilse
author_sort	Mandrini, Cristina Hemilse
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	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v728_n1_p_Torok http://hdl.handle.net/20.500.12110/paper_0004637X_v728_n1_p_Torok
work_keys_str_mv	AT mandrinicristinahemilse filamentinteractionmodeledbyfluxropereconnection
_version_	1768544390983188480

Filament interaction modeled by flux rope reconnection

Ejemplares similares