%0 Journal Article
%@holdercode {isadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S}
%@nexthigherunit 8JMKD3MGPCW/3EU29DP
%@resumeid 8JMKD3MGP5W/3C9JJ4U
%@archivingpolicy denypublisher denyfinaldraft12
%@usergroup administrator
%@usergroup marciana
%3 kane fluctuation.pdf
%X The number of coronal mass ejections (CMEs) erupting from the Sun follows a trend similar to that of sunspot numbers during the rising and maximum phase of the solar cycle. In the declining phase, the CME number has large fluctuations, dissimilar to those of sunspot numbers. In several studies of solar -aEuro parts per thousand interplanetary and solar -aEuro parts per thousand terrestrial relationships, the sunspot numbers and the 2800-MHz flux (F10) are used as representative of solar activity. In the rising phase, this may be adequate, but in the declining phase, solar parameters such as CMEs may have a different behaviour. Cosmic-ray Forbush decreases may occur even when sunspot activity is low. Therefore, when studying the solar influence on the Earth, one has to consider that although geomagnetic conditions at solar maximum will be disturbed, conditions at solar minimum may not be necessarily quiet.
%@mirrorrepository sid.inpe.br/mtc-m18@80/2008/03.17.15.17.24
%N 1
%T Fluctuations of Solar Activity during the Declining Phase of the 11-Year Sunspot Cycle
%@secondarytype PRE PI
%@visibility shown
%@group DGE-CEA-INPE-MCT-BR
%@secondarykey INPE--PRE/
%@issn 0038-0938
%@issn 1573-093X
%2 sid.inpe.br/mtc-m18@80/2009/07.20.11.47.03
%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
%B Solar Physics
%P 163-168
%4 sid.inpe.br/mtc-m18@80/2009/07.20.11.47
%D 2009
%V 255
%@doi 10.1007/s11207-008-9303-8
%O 0038-0938
%A Kane, Rajaram Purushottam,
%@dissemination WEBSCI; PORTALCAPES.
%@area CEA