@Article{Kane:2004:VaSoIn,
               author = "Kane, Rajaram Purushottam",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)}",
                title = "Variations of solar indices the sunspot maximum years (1999-2002) 
                         of cycle 23",
              journal = "Indian Journal of Radio and Space Physics",
                 year = "2004",
               volume = "33",
               number = "6",
                pages = "358--366",
                month = "Dec.",
             keywords = "solar indices, sunspot maximum, solar cycle 23.",
             abstract = "Comparison of the evolutions of daily and monthly values of 
                         several solar indices during 1999-2002 indicated that the daily 
                         values had large day-to-day fluctuations with peak spacings 
                         differing considerably from the 27-day solar rotation period. 
                         Plots of the percentage increases (trough-to-peak) versus 
                         temperature of the source regions of the various indices indicated 
                         a double-humped structure. The monthly values showed many peaks. 
                         The average spacing was -3.5 months (-100 days). The 12-month 
                         moving averages showed considerable differences. Some indices 
                         reached a maximum near March 2000. Some of these decreased since 
                         then and continue to decrease at present; but some reached a 
                         minimum near January 2001 and remained steady there, or started 
                         increasing again to reach a probable maximum near June 2002. Some 
                         indices did not have a maximum in March 2000 and continued to 
                         increase till June 2002. Thus, the evolutions of the various solar 
                         indices during the sunspot maximum of cycle 23 (1999-2002) are 
                         substantially different from each other. Obviously, the dynamical 
                         upheavals in the photosphere reach upper levels of the solar 
                         atmosphere with varying intensities.",
                 issn = "0367-8393 and 0975-105X",
             language = "en",
           targetfile = "IJRSP 33(6) 358-366.pdf",
        urlaccessdate = "04 maio 2024"
}