Relationships Among Magnetic Clouds, CMES, and Geomagnetic Storms |
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| Authors: | C C Wu R P Lepping N Gopalswamy |
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| Institution: | (1) CSPAR, University of Alabama, Huntsville, Alabama, 35899, U.S.A.;(2) Laboratory for Space Weather, Chinese Academy of Sciences, Beijing, P.R. China;(3) Heliophysics Science Division, NASA/GSFC, Greenbelt, Maryland, 20771, U.S.A.;(4) Solar System Exploration Division, NASA/GSFC, Greenbelt, Maryland, 20771, U.S.A. |
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| Abstract: | During solar cycle 23, 82 interplanetary magnetic clouds (MCs) were identified by the Magnetic Field Investigation (MFI) team
using Wind (1995 – 2003) solar wind plasma and magnetic field data from solar minimum through the maximum of cycle 23. The average occurrence
rate is 9.5 MCs per year for the overall period. It is found that some of the anomalies in the frequency of occurrence were
during the early part of solar cycle 23: (i) only four MCs were observed in 1999, and (ii) an unusually large number of MCs
(17 events) were observed in 1997, just after solar minimum. We also discuss the relationship between MCs, coronal mass ejections
(CMEs), and geomagnetic storms. During the period 1996 – 2003, almost 8000 CMEs were observed by SOHO-LASCO. The occurrence
frequency of MCs appears to be related neither to the occurrence of CMEs as observed by SOHO LASCO nor to the sunspot number.
When we included “magnetic cloud-like structures” (MCLs, defined by Lepping, Wu, and Berdichevsky, 2005), we found that the
occurrence of the joint set (MCs + MCLs) is correlated with both sunspot number and the occurrence rate of CMEs. The average
duration of the MCL structures is ~40% shorter than that of the MCs. The MCs are typically more geoeffective than the MCLs,
because the average southward field component is generally stronger and longer lasting in MCs than in MCLs. In addition, most
severe storms caused by MCs/MCLs with Dst
min≤ −100 nT occurred in the active solar period. |
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