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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. © 2010 Springer Science+Business Media B.V.

Registro:

Documento: Artículo
Título:Determining the Solar Source of a Magnetic Cloud Using a Velocity Difference Technique
Autor:Harra, L.K.; Mandrini, C.H.; Dasso, S.; Gulisano, A.M.; Steed, K.; Imada, S.
Filiación:UCL-Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey RH5 6NT, United Kingdom
Instituto de Astronomía y Física del Espacio, CONICET-UBA, 1428 Buenos Aires, Argentina
Facultad de Ciencias Exactas y Naturales, FCEN, UBA, CC. 67, Suc. 28, 1428 Buenos Aires, Argentina
Departamento de Física, FCEN, UBA, Buenos Aires, Argentina
Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara-shi, Kanagawa 229-8510, Japan
Palabras clave:Coronal mass ejections: interplanetary; Coronal mass ejections: low coronal signatures
Año:2010
Volumen:268
Número:1
Página de inicio:213
Página de fin:230
DOI: http://dx.doi.org/10.1007/s11207-010-9674-5
Título revista:Solar Physics
Título revista abreviado:Sol. Phys.
ISSN:00380938
Registro:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v268_n1_p213_Harra

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Citas:

---------- APA ----------
Harra, L.K., Mandrini, C.H., Dasso, S., Gulisano, A.M., Steed, K. & Imada, S. (2010) . Determining the Solar Source of a Magnetic Cloud Using a Velocity Difference Technique. Solar Physics, 268(1), 213-230.
http://dx.doi.org/10.1007/s11207-010-9674-5
---------- CHICAGO ----------
Harra, L.K., Mandrini, C.H., Dasso, S., Gulisano, A.M., Steed, K., Imada, S. "Determining the Solar Source of a Magnetic Cloud Using a Velocity Difference Technique" . Solar Physics 268, no. 1 (2010) : 213-230.
http://dx.doi.org/10.1007/s11207-010-9674-5
---------- MLA ----------
Harra, L.K., Mandrini, C.H., Dasso, S., Gulisano, A.M., Steed, K., Imada, S. "Determining the Solar Source of a Magnetic Cloud Using a Velocity Difference Technique" . Solar Physics, vol. 268, no. 1, 2010, pp. 213-230.
http://dx.doi.org/10.1007/s11207-010-9674-5
---------- VANCOUVER ----------
Harra, L.K., Mandrini, C.H., Dasso, S., Gulisano, A.M., Steed, K., Imada, S. Determining the Solar Source of a Magnetic Cloud Using a Velocity Difference Technique. Sol. Phys. 2010;268(1):213-230.
http://dx.doi.org/10.1007/s11207-010-9674-5