Relative occurrence rate and geoeffectiveness of large-scale types of the solar wind

Details Relative occurrence rate and geoeffectiveness of large-scale types of the solar wind Relative occurrence rate and geoeffectiveness of large-scale types of the solar wind

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010cosre..48....1y&link_type=abstract

Cosmic Research, Volume 48, Issue 1, pp.1-30

Physics

1

Scientific paper

We investigate the relative occurrence rate for various types of the solar wind and their geoeffectiveness for magnetic storms with Dst < —50 nT. Both integrated effect for the entire time 1976-2000 and variations during this period of 2.5 cycles of solar activity are studied As raw data for the analysis we have used the catalog of large-scale types of the solar wind for the period 1976-2000 (see ftp://ftp.iki.rssi.ru/omni/) created by us with the use of the OMNI database (http://omni.web.gsgc.nasa.gov) [1] and described in detail in [2]. The average annual numbers of different type of events are as follows: 124 ±81 for the heliospheric current sheet (HCS), 8 ±6 for magnetic clouds (MC), 99 ±38 for Ejecta, 46 ±19 for Sheath before Ejecta, 6 ±5 for Sheath before MC, and 63 ±15 for CIR. The measurements that allowed one to determine a source in the solar wind were available only for 58% of moderate and strong magnetic storms (with index Dst < —50 nT) during the period 1976-2000. Magnetic clouds (MC) are shown to be the most geoeffective (~61%). The CIR events and Ejecta with Sheath region are three times less geoeffective (~20-21 %). Variations of occurrence rate and geoeffectiveness of various types of the solar wind in the solar cycle are discussed.

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