Coronal Holes and Solar Wind High-Speed Streams: II. Forecasting the Geomagnetic Effects

Details Coronal Holes and Solar Wind High-Speed Streams: II. Forecasting the Geomagnetic Effects Coronal Holes and Solar Wind High-Speed Streams: II. Forecasting the Geomagnetic Effects

Feb 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007soph..240..331v&link_type=abstract

Solar Physics, Volume 240, Issue 2, pp.331-346

Physics

19

Scientific paper

We present a simple method of forecasting the geomagnetic storms caused by high-speed streams (HSSs) in the solar wind. The method is based on the empirical correlation between the coronal hole area/position and the value of the Dst index, which is established in a period of low interplanetary coronal mass ejection (ICME) activity. On average, the highest geomagnetic activity, i.e., the minimum in Dst, occurs four days after a low-latitude coronal hole (CH) crosses the central meridian. The amplitude of the Dst dip is correlated with the CH area and depends on the magnetic polarity of the CH due to the Russell McPherron effect. The Dst variation may be predicted by employing the expression Dst( t)=(-65±25×cos λ)[ A( t *)]0.5, where A( t *) is the fractional CH area measured in the central-meridian slice [-10°,10°] of the solar disc, λ is the ecliptic longitude of the Earth, ± stands for positive/negative CH polarity, and t- t *=4 days. In periods of low ICME activity, the proposed expression provides forecasting of the amplitude of the HSS-associated Dst dip to an accuracy of ≈30%. However, the time of occurrence of the Dst minimum cannot be predicted to better than ±2 days, and consequently, the overall mean relative difference between the observed and calculated daily values of Dst ranges around 50%.

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