Scatter in the plots of Dst(min) versus Bz(min)

Details Scatter in the plots of Dst(min) versus Bz(min) Scatter in the plots of Dst(min) versus Bz(min)

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010p%26ss...58.1792k&link_type=abstract

Planetary and Space Science, Volume 58, Issue 14-15, p. 1792-1801.

Physics

1

Scientific paper

In the plots of -Dst(min) versus -Bz(min) in cycle 23, in restricted ranges of -Dst(min), there was lot of scatter and the correlations were low. A bivariate analysis using geomagnetic -Dst(min) and auroral AE index did not improve the situation. Substitution of -Dst(min) by the ram-pressure-corrected true ring current Dst*(min) improved the correlations only slightly. Using the product V Bz instead of Bz(min) as a proxy for magnetospheric energy input did not improve the correlations, even for the 12 severe storm events in cycle 23. A multivariate analysis using -Bz(min) versus -Dst(min), with AU, AL and auroral particle precipitation index POES as additional indices improved the correlations and reduced the scatter. It was noticed, however, that for these severe storms, a major part of the solar wind input energy (˜85%) was still going to the Dst ring current, but this had an uncertainty of ˜15%. So in any severe storm event, the ring current could receive anything from 70% to 100% of the solar wind input energy.

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