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dc.contributor.author Harra, L. K.
dc.contributor.author Mandrini, Cristina Hemilse
dc.contributor.author Dasso, Sergio Ricardo
dc.contributor.author Gulisano, Adriana Maria
dc.contributor.author Steed, K.
dc.contributor.author Imada, S.
dc.date.available 2017-07-05T18:59:49Z
dc.date.issued 2011-01
dc.identifier.citation Harra, L. K.; Mandrini, Cristina Hemilse; Dasso, Sergio Ricardo; Gulisano, Adriana Maria; Steed, K.; et al.; Determining the solar source of a magnetic cloud using a velocity difference technique; Springer; Solar Physics; 268; 1; 1-2011; 213-230
dc.identifier.issn 0038-0938
dc.identifier.uri http://hdl.handle.net/11336/19633
dc.description.abstract For large eruptions on the Sun, it is often a problem that the core dimming region cannot be observed due to the bright emission from the flare itself. However, spectroscopic data can provide the missing information through the measurement of Doppler velocities. In this paper we analyse the well-studied flare and coronal mass ejection that erupted on the Sun on 13 December 2006 and reached the Earth on 14 December 2006. In this example, although the imaging data were saturated at the flare site itself, by using velocity measurements we could extract information on the core dimming region, as well as on remote dimmings. The purpose of this paper is to determine more accurately the magnetic flux of the solar source region, potentially involved in the ejection, through a new technique. The results of its application are compared to the flux in the magnetic cloud observed at 1 AU, as a way to check the reliability of this technique. We analysed data from the Hinode EUV Imaging Spectrometer to estimate the Doppler velocity in the active region and its surroundings before and after the event. This allowed us to determine a Doppler velocity ‘difference’ image. We used the velocity difference image overlayed on a Michelson Doppler Imager magnetogram to identify the regions in which the blue shifts were more prominent after the event; the magnetic flux in these regions was used as a proxy for the ejected flux and compared to the magnetic cloud flux. This new method provides a more accurate flux determination in the solar source region.
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
dc.subject LOW CORONAL SIGNATURES
dc.subject INTERPLANETARY MEDIUM
dc.subject.classification Astronomía
dc.subject.classification Ciencias Físicas
dc.subject.classification CIENCIAS NATURALES Y EXACTAS
dc.title Determining the solar source of a magnetic cloud using a velocity difference technique
dc.type info:eu-repo/semantics/article
dc.type info:ar-repo/semantics/artículo
dc.type info:eu-repo/semantics/publishedVersion
dc.date.updated 2017-07-05T15:46:58Z
dc.journal.volume 268
dc.journal.number 1
dc.journal.pagination 213-230
dc.journal.pais Alemania
dc.journal.ciudad Berlín
dc.description.fil Fil: Harra, L. K.. Mullard Space Science Laboratory; Reino Unido
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: Gulisano, Adriana Maria. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina
dc.description.fil Fil: Steed, K.. Mullard Space Science Laboratory; Reino Unido
dc.description.fil Fil: Imada, S.. Japan Aerospace Exploration Agency; Japón
dc.journal.title Solar Physics
dc.relation.alternativeid info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1007/s11207-010-9674-5
dc.relation.alternativeid info:eu-repo/semantics/altIdentifier/url/https://link.springer.com/article/10.1007/s11207-010-9674-5


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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)