On the variation of interplanetary magnetic cloud type through solar cycle 23: Wind events

Details On the variation of interplanetary magnetic cloud type through solar cycle 23: Wind events On the variation of interplanetary magnetic cloud type through solar cycle 23: Wind events

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jgra..11210103l&link_type=abstract

Journal of Geophysical Research, Volume 112, Issue A10, CiteID A10103

Physics

7

Interplanetary Physics: Ejecta, Driver Gases, And Magnetic Clouds, Interplanetary Physics: Interplanetary Magnetic Fields, Interplanetary Physics: Solar Cycle Variations (7536), Interplanetary Physics: Coronal Mass Ejections (7513)

Scientific paper

This statistical study examines the change in interplanetary magnetic cloud (MC) type, based on Wind observations of 100 MCs, taken during solar cycle 23 and split into three intervals: the minimum and rising phase of the cycle (over the years 1995-1998), the maximum phase (1999-2001), and the declining phase (2002 to early 2006). MC type refers to the profile of the latitude (or B Z , in geocentric solar ecliptic (GSE) coordinates) of the magnetic field within the MC, such as N-to-S (i.e., north-to-south from start to end), S-to-N, all S, almost all S, and so forth, with 10 categories in all. One of the main findings is that the strictly S-to-N events were very prevalent early in the cycle (i.e., 33% for the first phase) and tended to decrease in number as the cycle proceeded and that the strictly N-to-S cases had very low frequency of occurrence early in the cycle (i.e., 8% for the first phase) but tended to increase in number (22%) toward the end of the cycle, equal to the number of S-to-N events in that phase. When all S-to-N and N-to-S types for the full cycle are considered, the former clearly dominated over the latter by 1.4-to-1.

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