@Article{Kane:2006:CoVaCM,
               author = "Kane, Rajaram Purushottam",
          affiliation = "Instituto Nacional de Pesquisas Espaciais, Divis{\~a}o de 
                         Geof{\'{\i}}sica Espacial (INPE.DGE)",
                title = "Comparison of the Variations of CMEs and ICMEs with those of other 
                         Solar and Interplanetary Parameters During Solar Cycle 23",
              journal = "Solar Physics",
                 year = "2006",
               volume = "233",
               number = "1",
                pages = "107--115",
                month = "Jan.",
             abstract = "This paper examines the variations of coronal mass ejections 
                         (CMEs) and interplanetary CMEs (ICMEs) during solar cycle 23 and 
                         compares these with those of several other indices. During cycle 
                         23, solar and interplanetary parameters had an increase from 1996 
                         (sunspot minimum) to \∼2000, but the interval 19982002 had 
                         short-term fluctuations. Sunspot numbers had peaks in 1998, 1999, 
                         2000 (largest), 2001 (second largest), and 2002. Other solar 
                         indices had matching peaks, but the peak in 2000 was larger than 
                         the peak in 2001 only for a few indices, and smaller or equal for 
                         other solar indices. The solar open magnetic flux had very 
                         different characteristics for different solar latitudes. The high 
                         solar latitudes (45\∘90\∘) in both N and S 
                         hemispheres had flux evolutions anti-parallel to sunspot activity. 
                         Fluxes in low solar latitudes (0\∘45\∘) evolved 
                         roughly parallel to sunspot activity, but the finer structures 
                         (peaks etc. during sunspot maximum years) did not match with 
                         sunspot peaks. Also, the low latitude fluxes had considerable NS 
                         asymmetry. For CMEs and ICMEs, there were increases similar to 
                         sunspots during 19962000, and during 20002002, there was good 
                         matching of peaks. But the peaks in 2000 and 2001 for CMEs and 
                         ICMEs had similar sizes, in contrast to the 2000 peak being 
                         greater than the 2001 peak for sunspots. Whereas ICMEs started 
                         decreasing from 2001 onwards, CMEs continued to remain high in 
                         2002, probably due to extra contribution from high-latitude 
                         prominences, which had no equivalent interplanetary ICMEs or 
                         shocks. Cosmic ray intensity had features matching with those of 
                         sunspots during 20002001, with the 2000 peak (on a reverse scale, 
                         actually a cosmic ray decrease or trough) larger than the 2001 
                         peak. However, cosmic ray decreases started with a delay and ended 
                         with a delay with respect to sunspot activity.",
           copyholder = "SID/SCD",
                 issn = "0038-0938 and 1573-093X",
             language = "en",
           targetfile = "Comparison of the variations of CMEs and ICMEs.pdf",
        urlaccessdate = "14 maio 2024"
}