Statistical Comparison of Magnetic Clouds with Interplanetary Coronal Mass Ejections for Solar Cycle 23

Details Statistical Comparison of Magnetic Clouds with Interplanetary Coronal Mass Ejections for Solar Cycle 23 Statistical Comparison of Magnetic Clouds with Interplanetary Coronal Mass Ejections for Solar Cycle 23

Mar 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011soph..269..141w&link_type=abstract

Solar Physics, Volume 269, Issue 1, pp.141-153

Physics

3

Geomagnetic Storm, Interplanetary Coronal Mass Ejection, Magnetic Cloud, Solar Cycle

Scientific paper

We compare the number and characteristics of interplanetary coronal mass ejections (ICMEs) to those of magnetic clouds (MCs) by using in-situ solar wind plasma and magnetic field observations made at 1 AU during solar cycle 23. We found that ≈ 28% of ICMEs appear to contain MCs, since 103 magnetic clouds (MCs) occurred during 1995 - 2006, and 307 ICMEs occurred during 1996 - 2006. For the period between 1996 and 2006, 85 MCs are identified as part of ICMEs, and six MCs are not associated with ICMEs, which conflicts with the idea that MCs are usually a subset of ICMEs. It was also found that solar wind conditions inside MCs and ICMEs are usually similar, but the linear correlation between geomagnetic storm intensity ( Dst min ) and relevant solar wind parameters is better for MCs than for ICMEs. The differences between average event duration (Δ t) and average proton plasma β (< β>) are two of the major differences between MCs and ICMEs: i) the average duration of ICMEs (29.6 h) is 44% longer than for MCs (20.6 hours), and ii) the average of < β> is 0.01 for MCs and 0.24 for ICMEs. The difference between the definition of a MC and that for an ICME is one of the major reasons for these average characteristics being different ( i.e., listed above as items i) and ii)), and it is the reason for the frequency of their occurrences being different.

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