%0 Journal Article
%@holdercode {isadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S}
%@nexthigherunit 8JMKD3MGPCW/3EU29DP
%@archivingpolicy denypublisher denyfinaldraft24
%X 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 (not, vert, similar85%) was still going to the Dst ring current, but this had an uncertainty of not, vert, similar15%. So in any severe storm event, the ring current could receive anything from 70% to 100% of the solar wind input energy.
%@mirrorrepository sid.inpe.br/mtc-m19@80/2009/08.21.17.02.53
%8 Dec.
%N 14-15
%T Scatter in the plots of Dst(min) versus Bz(min)
%@secondarytype PRE PI
%K Scatter, Dst.
%@usergroup administrator
%@usergroup marciana
%@group DGE-CEA-INPE-MCT-BR
%3 kane.pdf
%@secondarykey INPE--PRE/
%@secondarymark B1_ASTRONOMIA_/_FÍSICA A2_GEOCIÊNCIAS B1_INTERDISCIPLINAR
%@issn 0032-0633
%2 sid.inpe.br/mtc-m19/2011/01.07.13.28.49
%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
%B Planetary and Space Science
%P 1792-1801
%4 sid.inpe.br/mtc-m19/2011/01.07.13.28
%D 2010
%V 58
%@doi 10.1016/j.pss.2010.07.026
%A Kane, R. P.,
%@dissemination WEBSCI; PORTALCAPES; COMPENDEX.
%@area CEA