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The link between CME-associated dimmings and interplanetary magnetic clouds

Published online by Cambridge University Press:  01 September 2008

Cristina H. Mandrini ,
María S. Nakwacki ,
Gemma Attrill ,
Lidia van Driel-Gesztelyi ,
Sergio Dasso  and
Pascal Démoulin
Cristina H. Mandrini
Affiliation:
Instituto de Astronomía y Física del Espacio, CC. 67 Suc. 28, 1428, Buenos Aires, Argentina email: mandrini@iafe.uba.ar
María S. Nakwacki
Affiliation:
Instituto de Astronomía y Física del Espacio, CC. 67 Suc. 28, 1428, Buenos Aires, Argentina email: mandrini@iafe.uba.ar
Gemma Attrill
Affiliation:
University College London, Mullard Space Science Laboratory, Holmbury St.Mary, Dorking, Surrey, RH5 6NT, UK Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA
Lidia van Driel-Gesztelyi
Affiliation:
University College London, Mullard Space Science Laboratory, Holmbury St.Mary, Dorking, Surrey, RH5 6NT, UK Observatoire de Paris, LESIA, UMR 8109 (CNRS), 92195 Meudon Principal Cedex, France Konkoly Observatory of the Hungarian Academy of Sciences, Budapest, Hungary
Sergio Dasso
Affiliation:
Instituto de Astronomía y Física del Espacio, CC. 67 Suc. 28, 1428, Buenos Aires, Argentina email: mandrini@iafe.uba.ar Departamento de Física, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires
Pascal Démoulin
Affiliation:
Observatoire de Paris, LESIA, UMR 8109 (CNRS), 92195 Meudon Principal Cedex, France
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Abstract

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Coronal dimmings often develop in the vicinity of erupting magnetic configurations. It has been suggested that they mark the location of the footpoints of ejected flux ropes and, thus, their magnetic flux can be used as a proxy for the ejected flux. If so, this quantity can be compared to the flux in the associated interplanetary magnetic cloud (MC) to find clues about the origin of the ejected flux rope. In the context of this interpretation, we present several events for which we have done a comparative solar-interplanetary analysis. We combine SOHO/Extreme Ultraviolet Imaging Telescope (EIT) data and Michelson Doppler Imager (MDI) magnetic maps to identify and measure the flux in the dimmed regions. We model the associated MCs and compute their magnetic flux using in situ observations. We find that the magnetic fluxes in the dimmings and MCs are compatible in some events; though this is not the case for large-scale and intense eruptions that occur in regions that are not isolated from others. We conclude that, in these particular cases, a fraction of the dimmed regions can be formed by reconnection between the erupting field and the surrounding magnetic structures, via a stepping process that can also explain other CME associated events.

Keywords

Sun: coronal mass ejections (CMEs)Sun: magnetic fieldsinterplanetary medium
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S257: Universal Heliophysical Processes , September 2008 , pp. 265 - 270
Copyright
Copyright © International Astronomical Union 2009

References

Attrill, G., Harra, L. K., van Driel-Gesztelyi, L., & Démoulin, P. 2007, ApJ, 656, L101.Google Scholar
Attrill, G., Nakwacki, M. S., Harra, L. K., van Driel-Gesztelyi, L., Mandrini, C. H., Dasso, S., & Wang, J. 2006, Solar Phys. 238, 117.CrossRefGoogle Scholar
Burlaga, L., Sittler, E., Mariani, F., & Schwenn, R. 1981, Jour. Geophys. Res., 86, 6673.CrossRefGoogle Scholar
Démoulin, P. 2007, An. Geo. 207, 87.Google Scholar
Hudson, H. S., Acton, L. W., & Freeland, S. L. 1996, ApJ 470, 629.CrossRefGoogle Scholar
Lin, J. & Forbes, T. G. 2000, Jour. Geophys. Res. 105, 2375.CrossRefGoogle Scholar
Mandrini, C. H., Nakwacki, M. S., Attrill, G., van Driel-Gesztelyi, L., Démoulin, P., Dasso, S., & Elliott, H. 2007, Solar Phys., 244, 25.CrossRefGoogle Scholar
Mandrini, C. H., Pohjolainen, S., Dasso, S., Green, L. M., Démoulin, P., van Driel-Gesztelyi, L., Copperwheat, C., & Foley, C. 2005, A&A, 434, 725.Google Scholar
Qiu, J., Hu, Q., Howard, T. A., & Yurchyshyn, V. B. 2007, ApJ, 659, 758.CrossRefGoogle Scholar
Webb, D. F., Lepping, R. P., Burlaga, L. F., DeForest, C. E., Larson, D. E., Martin, S. F., Plunkett, S. P., & Rust, D. M. 2000, Jour. Geophys. Res., 105, 27251.CrossRefGoogle Scholar