%0 Journal Article %@holdercode {isadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S} %@nexthigherunit 8JMKD3MGPCW/3EU29DP %@archivingpolicy denypublisher denyfinaldraft12 %@issn 0038-0938 %@issn 1573-093X %@usergroup administrator %@usergroup simone %3 gnevyshev.pdf %2 sid.inpe.br/mtc-m17@80/2008/06.18.12.23.13 %4 sid.inpe.br/mtc-m17@80/2008/06.18.12.23 %X The sunspot number series at the peak of sunspot activity often has two or three peaks (Gnevyshev peaks; Gnevyshev, Solar Phys. 1, 107, 1967; Solar Phys. 51, 175, 1977). The sunspot group number (SGN) data were examined for 1997  2003 (part of cycle 23) and compared with data for coronal mass ejection (CME) events. It was noticed that they exhibited mostly two Gnevyshev peaks in each of the four latitude belts 0°  10°, 10°  20°, 20 °  30°, and > 30°, in both N (northern) and S (southern) solar hemispheres. The SGN were confined to within latitudes ± 50° around the Equator, mostly around ± 35°, and seemed to occur later in lower latitudes, indicating possible latitudinal migration as in the Maunder butterfly diagrams. In CMEs, less energetic CMEs (of widths < 71°) showed prominent Gnevyshev peaks during sunspot maximum years in almost all latitude belts, including near the poles. The CME activity lasted longer than the SGN activity. However, the CME peaks did not match the SGN peaks and were almost simultaneous at different latitudes, indicating no latitudinal migration. In energetic CMEs including halo CMEs, the Gnevyshev peaks were obscure and ill-defined. The solar polar magnetic fields show polarity reversal during sunspot maximum years, first at the North Pole and, a few months later, at the South Pole. However, the CME peaks and gaps did not match with the magnetic field reversal times, preceding them by several months, rendering any cause  effect relationship doubtful. %8 June %N 2 %T Gnevyshev Peaks and Gaps for Coronal Mass Ejections of Different Widths Originating in Different Solar Position Angles %@secondarytype PRE PI %@group DGE-CEA-INPE-MCT-BR %@secondarykey INPE--PRE/ %@affiliation Instituto Nacional de Pesquisas Espaciais (INPE) %B Solar Physics %P 369-380 %D 2008 %V 249 %@doi 10.1007/s11207-008-9185-9 %A Kane, Rajaram Purushotam, %@dissemination WEBSCI; PORTALCAPES. %@area CEA