TitleStatistical study of magnetic cloud erosion by magnetic reconnection
Publication TypeJournal Article
Year of Publication2015
AuthorsRuffenach, A, Lavraud, B, Farrugia, CJ, émoulin, P, Dasso, S, Owens, MJ, Sauvaud, J-A, Rouillard, AP, Lynnyk, A, Foullon, C, Savani, NP, Luhmann, JG, Galvin, AB
JournalJournal of Geophysical Research: Space Physics
Volume120136149386113144552445075509811325259136228017217110111401955610315391362287256119957
Issue1A7A81-22A3A9151-21-41-471-43A21-2A811-41-2A411027073A1015-1622221A6
Pagination43 - 60
Date Published01/2015
Keywordscoronal mass ejection; magnetic cloud; magnetic flux rope; magnetic reconnection; parker solar probe; Solar Probe Plus; Solar wind
Abstract

recent studies suggest that magnetic reconnection is able to erode substantial amounts of the outer magnetic flux of interplanetary magnetic clouds (MCs) as they propagate in the heliosphere. We quantify and provide a broader context to this process, starting from 263 tabulated interplanetary coronal mass ejections, including MCs, observed over a time period covering 17 years and at a distance of 1 AU from the Sun with Wind (1995-2008) and the two STEREO (2009-2012) spacecraft. Based on several quality factors, including careful determination of the MC boundaries and main magnetic flux rope axes, an analysis of the azimuthal flux imbalance expected from erosion by magnetic reconnection was performed on a subset of 50 MCs. The results suggest that MCs may be eroded at the front or at rear and in similar proportions, with a significant average erosion of about 40% of the total azimuthal magnetic flux. We also searched for in situ signatures of magnetic reconnection causing erosion at the front and rear boundaries of these MCs. Nearly ~30% of the selected MC boundaries show reconnection signatures. Given that observations were acquired only at 1 AU and that MCs are large-scale structures, this finding is also consistent with the idea that erosion is a common process. Finally, we studied potential correlations between the amount of eroded azimuthal magnetic flux and various parameters such as local magnetic shear, Alfvén speed, and leading and trailing ambient solar wind speeds. However, no significant correlations were found, suggesting that the locally observed parameters at 1 AU are not likely to be representative of the conditions that prevailed during the erosion which occurred during propagation from the Sun to 1 AU. Future heliospheric missions, and in particular Solar Orbiter or Solar Probe Plus, will be fully geared to answer such questions.

URLhttp://doi.wiley.com/10.1002/2014JA020628http://onlinelibrary.wiley.com/wol1/doi/10.1002/2014JA020628/fullpdf
DOI10.1002/2014JA020628
Short TitleJ. Geophys. Res. Space Physics


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