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dc.contributor.author Gibson, S. E.
dc.contributor.author Fan, Y.
dc.contributor.author Mandrini, Cristina Hemilse
dc.contributor.author Fisher, G.
dc.contributor.author Démoulin, Pascal
dc.date.available 2017-07-24T17:59:40Z
dc.date.issued 2004-12
dc.identifier.citation Gibson, S. E.; Fan, Y.; Mandrini, Cristina Hemilse; Fisher, G.; Démoulin, Pascal; Observational consequences of a magnetic flux rope emerging into the corona; IOP Publishing; Astrophysical Journal; 617; 1; 12-2004; 600-613
dc.identifier.issn 0004-637X
dc.identifier.uri http://hdl.handle.net/11336/21173
dc.description.abstract We show that a numerical simulation of a magnetic flux rope emerging into a coronal magnetic field predicts solar structures and dynamics consistent with observations. We first consider the structure, evolution, and relative location and orientation of S-shaped, or sigmoid, active regions and filaments. The basic assumptions are that (1) X-ray sigmoids appear at the regions of the flux rope known as ``bald-patch-associated separatrix surfaces (BPSSs), where, under dynamic forcing, current sheets can form, leading to reconnection and localized heating, and that (2) filaments are regions of enhanced density contained within dips in the magnetic flux rope. We demonstrate that the shapes and relative orientations and locations of the BPSS and dipped field are consistent with observations of X-ray sigmoids and their associated filaments. Moreover, we show that current layers indeed form along the sigmoidal BPSS as the flux rope is driven by the kink instability. Finally, we consider how apparent horizontal motions of magnetic elements at the photosphere caused by the emerging flux rope might be interpreted. In particular, we show that local correlation tracking analysis of a time series of magnetograms for our simulation leads to an underestimate of the amount of magnetic helicity transported into the corona by the flux rope, largely because of undetectable twisting motions along the magnetic flux surfaces. Observations of rotating sunspots may provide better information about such rotational motions, and we show that if we consider the separated flux rope legs as proxies for fully formed sunspots, the amount of rotation that would be observed before the region becomes kink unstable would be in the range 40°-200° per leg/sunspot, consistent with observations.
dc.format application/pdf
dc.language.iso eng
dc.publisher IOP Publishing
dc.rights info:eu-repo/semantics/restrictedAccess
dc.rights.uri https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject.classification Astronomía
dc.subject.classification Ciencias Físicas
dc.subject.classification CIENCIAS NATURALES Y EXACTAS
dc.title Observational consequences of a magnetic flux rope emerging into the corona
dc.type info:eu-repo/semantics/article
dc.type info:ar-repo/semantics/artículo
dc.type info:eu-repo/semantics/publishedVersion
dc.date.updated 2017-07-24T14:12:30Z
dc.journal.volume 617
dc.journal.number 1
dc.journal.pagination 600-613
dc.journal.pais Reino Unido
dc.journal.ciudad Londres
dc.description.fil Fil: Gibson, S. E.. National Center for Atmospheric Research; Estados Unidos
dc.description.fil Fil: Fan, Y.. National Center for Atmospheric Research; 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.description.fil Fil: Fisher, G.. Space Science Laboratories; Estados Unidos
dc.description.fil Fil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
dc.journal.title Astrophysical Journal
dc.relation.alternativeid info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1086/425294/meta
dc.relation.alternativeid info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1086/425294


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info:eu-repo/semantics/restrictedAccess Excepto donde se diga explícitamente, este item se publica bajo la siguiente descripción: Creative Commons Attribution-NonCommercial-ShareAlike 2.5 Unported (CC BY-NC-SA 2.5)