Physics of auroral phenomena : proceedings of the 37th Annual seminar, Apatity, 25 - 28 February, 2014 / [ed. board: A. G. Yahnin, N. V. Semenova]. - Апатиты : Изд-во Кольского научного центра РАН, 2014. - 125 с. : ил., табл.

N.G. Kleimenova et al. I S E S S o la r Cy cl e S u n s p o t N u m b e r P r o g r e s s io n O b s e r v e d data th r o u g h Jui 2 0 1 3 U o d a tn d 2 0 1 3 Au<i S N O A A /S W P C B o u ld e r .C O U S A Figure 1. The solar activity (measured the Sunspot number) in 2001-2013 (blue line) and its prediction (red line). The common yearly Pci duration (the number of the hours with long-lasting Pci series during one year) in the declining phase of the 23-th cycle of the solar activity (2006), was rather high -270, but in 2008, this number was -100 and in 2009 it was only -20. 0АЧЯ«ДО№№КМ«ТЕЯМ1 v ____м_____ __ ____ _____________ ют :"VT f i‘ T i ТУ »'T ’£*TiV'i ГТГТ'й’Т'чТ^^ГиТ'й'Т ж” m’ » Г* ГйГГаГПт's ти I» Г. ' I a k a J . шЯш » И* \ .,%». ч ^ t м‘“ •*** V , „Т f t * 9 •• v % » « » *е J fM т .£» " ** №К -Д .у> . . . » ♦ /,■•* V VА . -------- -ftI■щипЛл } fy, т 10 " |^“1*о <л Л *. j . y.vN^ ^ ^ '|V»»ti * «Jw -■-:~т -~ ’V4*' у‘ ' • 'и^ок -ь у . у ли <*. „ *&*•< 4 й 4 « и ^ . PLANETARY MAGNETIC THREE-HOURRANGE INDICES Kp 2008 : К=ЛI Я !» :NI» • Л ... JS^j^^Aj^L^SAjLsSu -- t i у , rfi & , C?iT* ins £ !!ЗГ . «f: Чч^чи ..iillll PLANETARYMAGNETIC THREE-HOUR-fiANGE INDICES Kp 2009 Figure 2.The geomagnetic activity and long-lasting Pci occurrence (red bars) in 2008 and 2009 The spectral structure of the Pci pulsations was different in quiet and disturbed magnetic conditions. It was much more complicated under the latest (see some examples in Fig. 3). As a rule, during the solar activity minimum, the shape of the frequency-temporal Pci spectra looked like a very monochromatic emission o f not more 3-5 hours duration with a narrow of the width of the dynamic spectra. An example of such event is presented at the right panel of Fig. 3 (on 30.07.2009 under Kp-0-1). The central frequency of the Pci emissions was less 1 Hz with the spectral width in the order o f 0.2-0.3 Hz. During the declining (2006) and increasing (2010) phases of the solar activity, the spectral structure of Pci pulsations became more complicated and the duration of the Pci series increased up to 10-12 hours. Sometimes it 64