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Reconnection in a Slow Coronal Mass Ejection : Volume 26, Issue 10 (15/10/2008)

By Poletto, G.

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Book Id: WPLBN0004001900
Format Type: PDF Article :
File Size: Pages 9
Reproduction Date: 2015

Title: Reconnection in a Slow Coronal Mass Ejection : Volume 26, Issue 10 (15/10/2008)  
Author: Poletto, G.
Volume: Vol. 26, Issue 10
Language: English
Subject: Science, Annales, Geophysicae
Collections: Periodicals: Journal and Magazine Collection (Contemporary), Copernicus GmbH
Historic
Publication Date:
2008
Publisher: Copernicus Gmbh, Göttingen, Germany
Member Page: Copernicus Publications

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Romoli, M., Landini, F., Bemporad, A., & Poletto, G. (2008). Reconnection in a Slow Coronal Mass Ejection : Volume 26, Issue 10 (15/10/2008). Retrieved from http://members.worldlibrary.net/


Description
Description: INAF – Arcetri Astrophysical Observatory, Firenze, Italy. This paper aims at studying reconnection occurring in the aftermath of the 28 May 2004, CME, first imaged by the LASCO (Large Angle and Spectrometric Coronagraph) C2 at 11:06 UT. The CME was observed in White Light and UV radiation: images acquired by the LASCO C2 and C3 coronagraphs and spectra acquired by UVCS (Ultraviolet Coronagraph Spectrometer) allowed us to identify the level at which field lines, stretched outwards by the CME ejection, reconnect below the CME bubble. As the CME propagates outwards, reconnection occurs at increasingly higher levels. The process goes on at a low pace for several hours: here we give the profile of the reconnection rate vs. heliocentric distance over a time interval of ≈14 h after the CME onset, extending estimates of the reconnection rate to larger distances than previously inferred by other authors. The reconnection rate appears to decrease with time/altitude. We also calculate upper and lower limits to the density in the diffusion region between 4 and 7 R and conclude by comparing estimates of the classical and anomalous resistivity in the diffusion region with the value inferred from the data. The latter turns out to be ≥5 order of magnitudes larger than predicted by classical or anomalous theories, pointing to the need of identifying the process responsible for the observed value.

Summary
Reconnection in a slow Coronal Mass Ejection

Excerpt
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