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dc.contributor.author
Harra, L. K.  
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Mandrini, Cristina Hemilse  
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Dasso, Sergio Ricardo  
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Gulisano, Adriana Maria  
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Steed, K.  
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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  
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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.  
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application/pdf  
dc.language.iso
eng  
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Springer  
dc.rights
info:eu-repo/semantics/restrictedAccess  
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https://creativecommons.org/licenses/by-nc-sa/2.5/ar/  
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Coronal Mass Ejections  
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Low Coronal Signatures  
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Interplanetary Medium  
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Astronomía  
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Ciencias Físicas  
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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  
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info:ar-repo/semantics/artículo  
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info:eu-repo/semantics/publishedVersion  
dc.date.updated
2017-07-05T15:46:58Z  
dc.journal.volume
268  
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1  
dc.journal.pagination
213-230  
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Alemania  
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Berlín  
dc.description.fil
Fil: Harra, L. K.. Mullard Space Science Laboratory; Reino Unido  
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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  
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Fil: Gulisano, Adriana Maria. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina  
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Fil: Steed, K.. Mullard Space Science Laboratory; Reino Unido  
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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  
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info:eu-repo/semantics/altIdentifier/url/https://link.springer.com/article/10.1007/s11207-010-9674-5