%0 Journal Article
%@holdercode {isadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S}
%@nexthigherunit 8JMKD3MGPCW/3EU29DP
%@archivingpolicy denypublisher denyfinaldraft12
%@usergroup administrator
%@usergroup simone
%3 similarities.pdf
%2 sid.inpe.br/mtc-m17@80/2008/06.05.18.37.21
%4 sid.inpe.br/mtc-m17@80/2008/06.05.18.37
%X From the LASCO CME (Coronal Mass Ejection) catalog, the occurrence frequencies of all CMEs (all strong and weak CMEs, irrespective of their widths) were calculated for 3-month intervals and their 12-month running means determined for cycle 23 (1996-2007) and were compared with those of other solar parameters. The annual values of all-CME frequency were very well correlated (+ 0.97) with sunspot numbers, but several other parameters also had similarly high correlations. Comparisons of 12-month running means indicated that the sunspot numbers were very well correlated with solar electromagnetic radiations (Lyman-alpha, 2800-MHz flux, coronal green line index, solar flare indices, and X-ray background); but for corpuscular radiations [proton fluxes, solar energetic particles (SEP), CMEs, interplanetary CMEs (ICMEs), and stream interaction regions (SIR)] and solar open magnetic fields, the correlations were lower. A notable feature was the appearance of two peaks during 2000-2002, and those double peaks in different parameters matched approximately except for proton fluxes and SEP and SIR frequencies. When hemispheric intensities were considered, north-south asymmetries appeared, more in some parameters than in others. When intensities in smaller latitude belts (10 degrees) were compared, sunspot group numbers (SGN) were found to be confined mostly to latitudes within +/- 30 degrees of the solar equator, showing two peaks in all latitude belts, and during the course of the 11-year cycle, the double peaks shifted from middle to equatorial solar latitudes, just as seen in the Maunder butterfly diagrams. In contrast, CME frequency was comparable at all latitude belts (including high, near-polar latitudes), having more than two peaks in almost all latitude belts, and the peaks were almost simultaneous in all latitude belts. Thus, the matching of SGN peaks with those of CME peaks was poor. Incidentally, the CME frequency data for all events (all widths) after 2003 are not comparable to earlier data, owing to inclusion of very weak (narrow) CMEs in later years. The frequencies are comparable with earlier data only for widths exceeding about 70(degrees).
%8 Mar.
%N 1
%T Similarities and Dissimilarities between the Variations of CME and Other Solar Parameters at Different Heliographic Latitudes and Time Scales
%@secondarytype PRE PI
%K CORONAL MASS EJECTIONS, GROUP SUNSPOT NUMBERS, ACTIVITY RECONSTRUCTION, CYCLE VARIATION, INDEXES, FLUX.
%@group DGE-CEA-INPE-MCT-BR
%@secondarykey INPE--PRE/
%@issn 0038-0938
%@issn 1573-093X
%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
%B Solar Physics
%P 177-190
%D 2008
%V 248
%@doi 10.1007/s11207-008-9145-4
%A Kane, Rajaram Purushotam,
%@dissemination WEBSCI; PORTALCAPES.
%@area CEA