%0 Journal Article
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%@nexthigherunit 8JMKD3MGPCW/3EU29DP
%@resumeid 8JMKD3MGP5W/3C9JJ4U
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%3 kane3.pdf
%X Sunspots have a major 11-year cycle, but the three to four years near the maximum may show two or more peaks called Gnevyshev peaks. Earlier, it was reported that in Solar Cycle 23, the double peak in sunspot numbers was reflected in the electromagnetic radiations and coronal mass ejection (CME) frequencies in the solar atmosphere, but with phase differences. In this article, it is shown that the average CME speeds also show Gnevyshev peaks but with phase differences.
%@mirrorrepository sid.inpe.br/mtc-m19@80/2009/08.21.17.02.53
%8 JAN
%N 1
%T Gnevyshev Peaks in the CME Average Speeds in Cycle 23
%@secondarytype PRE PI
%K Gnevyshev peaks, Cycle 23 coronal mass ejections, cosmic-ray modulation, solar-cycle, latitude dependence, magnetic-field, parameters, events, gaps.
%@usergroup administrator
%@usergroup marciana
%@group DGE-CEA-INPE-MCT-BR
%@secondarykey INPE--PRE/
%@issn 0038-0938
%@issn 1573-093X
%2 sid.inpe.br/mtc-m19@80/2010/07.29.13.59.53
%@project FNDCT, Brazil [FINEP-537/CT]
%B Solar Physics
%P 209-213
%4 sid.inpe.br/mtc-m19@80/2010/07.29.13.59
%D 2010
%V 261
%@doi 10.1007/s11207-009-9466-y
%A Kane, Rajaram Purushottam,
%@dissemination WEBSCI; PORTALCAPES.
%@area CEA