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Cluster-c1 Observations on the Geometrical Structure of Linear Magnetic Holes in the Solar Wind at 1 Au : Volume 28, Issue 9 (20/09/2010)

By Xiao, T.

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Book Id: WPLBN0003983537
Format Type: PDF Article :
File Size: Pages 8
Reproduction Date: 2015

Title: Cluster-c1 Observations on the Geometrical Structure of Linear Magnetic Holes in the Solar Wind at 1 Au : Volume 28, Issue 9 (20/09/2010)  
Author: Xiao, T.
Volume: Vol. 28, Issue 9
Language: English
Subject: Science, Annales, Geophysicae
Collections: Periodicals: Journal and Magazine Collection (Contemporary), Copernicus GmbH
Historic
Publication Date:
2010
Publisher: Copernicus Gmbh, Göttingen, Germany
Member Page: Copernicus Publications

Citation

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Zong, Q. G., Shi, Q. Q., Xiao, T., Zhang, T. L., Fu, S. Y., Pu, Z. Y.,...Sun, W. J. (2010). Cluster-c1 Observations on the Geometrical Structure of Linear Magnetic Holes in the Solar Wind at 1 Au : Volume 28, Issue 9 (20/09/2010). Retrieved from http://www.ebooklibrary.org/


Description
Description: School of Space Science and Physics, Shandong University at Weihai, Weihai, China. Interplanetary linear magnetic holes (LMHs) are structures in which the magnetic field magnitude decreases with little change in the field direction. They are a 10–30% subset of all interplanetary magnetic holes (MHs). Using magnetic field and plasma measurements obtained by Cluster-C1, we surveyed the LMHs in the solar wind at 1 AU. In total 567 interplanetary LMHs are identified from the magnetic field data when Cluster-C1 was in the solar wind from 2001 to 2004. We studied the relationship between the durations and the magnetic field orientations, as well as that of the scales and the field orientations of LMHs in the solar wind. It is found that the geometrical structure of the LMHs in the solar wind at 1 AU is consistent with rotational ellipsoid and the ratio of scales along and across the magnetic field is about 1.93:1. In other words, the structure is elongated along the magnetic field at 1 AU. The occurrence rate of LMHs in the solar wind at 1 AU is about 3.7 per day. It is shown that not only the occurrence rate but also the geometrical shape of interplanetary LMHs has no significant change from 0.72 AU to 1 AU in comparison with previous studies. It is thus inferred that most of interplanetary LMHs observed at 1 AU are formed and fully developed before 0.72 AU. The present results help us to study the formation mechanism of the LMHs in the solar wind.

Summary
Cluster-C1 observations on the geometrical structure of linear magnetic holes in the solar wind at 1 AU

Excerpt
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