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dc.contributor.author
Török, T.
dc.contributor.author
Chandra, R.
dc.contributor.author
Pariat, E.
dc.contributor.author
Démoulin, Pascal
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dc.contributor.author
Schmieder, B.
dc.contributor.author
Aulanier, G.
dc.contributor.author
Linton, M.
dc.contributor.author
Mandrini, Cristina Hemilse
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dc.date.available
2017-07-05T18:27:11Z
dc.date.issued
2011-02
dc.identifier.citation
Török, T.; Chandra, R.; Pariat, E.; Démoulin, Pascal; Schmieder, B.; et al.; Filament interaction modeled by flux rope reconnection; IOP Publishing; Astrophysical Journal; 728; 1; 2-2011; 1-6; 65
dc.identifier.issn
0004-637X
dc.identifier.uri
http://hdl.handle.net/11336/19621
dc.description.abstract
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 Demoulin 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.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
IOP Publishing
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dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
Sun - Corona
dc.subject
Sun - Prominences -Filaments
dc.subject
Numerical Methods
dc.subject.classification
Astronomía
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dc.subject.classification
Ciencias Físicas
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dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
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dc.title
Filament interaction modeled by flux rope reconnection
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2017-07-05T15:47:01Z
dc.journal.volume
728
dc.journal.number
1
dc.journal.pagination
1-6; 65
dc.journal.pais
Reino Unido
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dc.journal.ciudad
Londres
dc.description.fil
Fil: Török, T.. Université Paris Diderot - Paris 7; Francia
dc.description.fil
Fil: Chandra, R.. Université Paris Diderot - Paris 7; Francia
dc.description.fil
Fil: Pariat, E.. Université Paris Diderot - Paris 7; Francia
dc.description.fil
Fil: Démoulin, Pascal. Université Paris Diderot - Paris 7; Francia
dc.description.fil
Fil: Schmieder, B.. Université Paris Diderot - Paris 7; Francia
dc.description.fil
Fil: Aulanier, G.. Université Paris Diderot - Paris 7; Francia
dc.description.fil
Fil: Linton, M.. Spece Sciences División. Naval Research Laboratory; Estados Unidos
dc.description.fil
Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
dc.journal.title
Astrophysical Journal
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dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1088/0004-637X/728/1/65
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-637X/728/1/65/meta
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