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dc.contributor.author Webb, D. F.
dc.contributor.author Cremades Fernandez, Maria Hebe
dc.contributor.author Sterling, A. C.
dc.contributor.author Mandrini, Cristina Hemilse
dc.contributor.author Dasso, Sergio Ricardo
dc.contributor.author Gibson, S. E.
dc.contributor.author Haber, D. A.
dc.contributor.author Komm, R. W.
dc.contributor.author Petrie, G. J. D.
dc.contributor.author McIntosh, P. S.
dc.contributor.author Welsch, B. T.
dc.contributor.author Plunkett, S. P.
dc.date.available 2017-07-10T18:16:47Z
dc.date.issued 2011-12
dc.identifier.citation Webb, D. F.; Cremades Fernandez, Maria Hebe; Sterling, A. C.; Mandrini, Cristina Hemilse; Dasso, Sergio Ricardo; et al.; The Global Context of Solar Activity During the Whole Heliosphere Interval Campaign; Springer; Solar Physics; 274; 1-2; 12-2011; 57-86
dc.identifier.issn 0038-0938
dc.identifier.uri http://hdl.handle.net/11336/20005
dc.description.abstract The Whole Heliosphere Interval (WHI) was an international observing and modeling effort to characterize the 3-D interconnected “heliophysical” system during this solar minimum, centered on Carrington Rotation 2068, March 20 – April 16, 2008. During the latter half of the WHI period, the Sun presented a sunspot-free, deep solar minimum type face. But during the first half of CR 2068 three solar active regions flanked by two opposite-polarity, low-latitude coronal holes were present. These departures from the quiet Sun led to both eruptive activity and solar wind structure. Most of the eruptive activity, i.e., flares, filament eruptions and coronal mass ejections (CMEs), occurred during this first, active half of the interval. We determined the source locations of the CMEs and the type of associated region, such as active region, or quiet sun or active region prominence. To analyze the evolution of the events in the context of the global solar magnetic field and its evolution during the three rotations centered on CR 2068, we plotted the CME source locations onto synoptic maps of the photospheric magnetic field, of the magnetic and chromospheric structure, of the white light corona, and of helioseismological subsurface flows. Most of the CME sources were associated with the three dominant active regions on CR 2068, particularly AR 10989. Most of the other sources on all three CRs appear to have been associated with either isolated filaments or filaments in the north polar crown filament channel. Although calculations of the flux balance and helicity of the surface magnetic features did not clearly identify a dominance of one region over the others, helioseismological subsurface flows beneath these active regions did reveal a pronounced difference among them. These preliminary results suggest that the “twistedness” (i.e., vorticity and helicity) of subsurface flows and its temporal variation might be related to the CME productivity of active regions, similar to the relationship between flares and subsurface flows.
dc.format application/pdf
dc.language.iso eng
dc.publisher Springer
dc.rights info:eu-repo/semantics/restrictedAccess
dc.rights.uri https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject CORONAL MASS EJECTIONS: ORIGIN
dc.subject SOLAR SYNOPTIC MAPS
dc.subject HELIOSEISMOLOGY
dc.subject SUBSURFACE FLOWS
dc.subject.classification Astronomía
dc.subject.classification Ciencias Físicas
dc.subject.classification CIENCIAS NATURALES Y EXACTAS
dc.title The Global Context of Solar Activity During the Whole Heliosphere Interval Campaign
dc.type info:eu-repo/semantics/article
dc.type info:ar-repo/semantics/artículo
dc.type info:eu-repo/semantics/publishedVersion
dc.date.updated 2017-07-10T13:26:16Z
dc.journal.volume 274
dc.journal.number 1-2
dc.journal.pagination 57-86
dc.journal.pais Alemania
dc.journal.ciudad Berlín
dc.description.fil Fil: Webb, D. F.. Boston College; Estados Unidos
dc.description.fil Fil: Cremades Fernandez, Maria Hebe. Universidad Tecnologica Nacional; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
dc.description.fil Fil: Sterling, A. C.. National Aeronautics And Space Administration; 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: Dasso, Sergio Ricardo. 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: Gibson, S. E.. High Altitude Observatory; Estados Unidos
dc.description.fil Fil: Haber, D. A.. State University Of Colorado Boulder; Estados Unidos
dc.description.fil Fil: Komm, R. W.. National Solar Observatory; Estados Unidos
dc.description.fil Fil: Petrie, G. J. D.. National Solar Observatory; Estados Unidos
dc.description.fil Fil: McIntosh, P. S.. Heliosynoptics; Estados Unidos
dc.description.fil Fil: Welsch, B. T.. University of California; Estados Unidos
dc.description.fil Fil: Plunkett, S. P.. Spece Sciences División. Naval Research Laboratory; Estados Unidos
dc.journal.title Solar Physics
dc.relation.alternativeid info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1007/s11207-011-9787-5
dc.relation.alternativeid info:eu-repo/semantics/altIdentifier/url/https://link.springer.com/article/10.1007/s11207-011-9787-5


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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)