Авроральные явления - 75 : материалы наблюдений Полярного геофизического института за 1975 г. / Акад. наук СССР, Кол. фил. им. С. М. Кирова, Поляр. геофиз. ин-т ; [редкол.: Б. Е. Брюнелли (отв. ред.) и др.]. - Апатиты : Кольский филиал АН СССР, 1978.

4 AUHOHAL PHENOMENA - 75 The Observational Data of the Polar Ueophysical Institute Academy of Sciences of the USSR Editor B.E.Brunelli Apatity - 1978 The volume contains t h e o b s e r v a t i o n a l data o f g e o p h y s i c a l p r o c e s s e s o v e r t h e Coxa peninsula in 1975« The r e p o r t continues the series s t a r t e d i n 1970 and h a s t h e form similar со one o f the previous v o l u m e s . T h e data are p r e p a r e d b y G.A. .Loginov, Jj.T.Afanasoeva (geomagnetism), N . Y . a h u i g i n a , К.И.лшсизйкта ( i o n o s p h e r e ; , L.S. Evlashin, a.V.StarKov, G.ii' .Totunova ( a u r o r a s J, O.A.Mexnikov ( D a i o o n d a t a ) . T h e activity description was aone D y B.ii.ttruheiil a n a G.V.Starkov. T h e v o l u m e i s prepared t o publication b y L.V. K o v a l e v s k a y a . The x-eport contains the dace - the magnetograms (H-component) at st.Loparskaya (in some cases - s t 0 Lovozero); coordinates are given in Introduction, page 3» - the hourly range (Гп) tables (Lopa.t :aya), -- the graphs of riometer absorption (in dB, riometer 32 MHz, .boparsfcaya, antenna 50x 60° is directed to the Polar star) - the ascaplots based on the data < all-зку G- 1 S 0 camera (LoparsKaya), - the main auroral emission intensity, - the time and counting rate of the baloon flights (Apatity), The universal time are used everywhere. Sometimes che midnight, sunrise and sun set are also given. The local midnight for the Coxa peninsula is 22 UT. The local geomagnetic midnight corresponds to 21.01, 2 0 ,43 and 21.19 lit at equinox and near June and December solstices. The ascaplots are presented as usual, for each naif an nour interval (+15 min from tne pointed value) aurora occurence in the northern, zenith and southern directions a:ce given on unroe upper lines» t o denote aurora intensity in the zenith direction more tnan class .1 two lower lines are used. (Jlouoness (partial or complete) is marJtea by dots or vertical line respectively, rue time or appearance 01 cne moon is шагкеа oy horizoncai line over grapn. m e spectral lines А=4276» 5577, 63 ОО and 6789 $ emission intensities (in b class scale) and the transparence values: A -good transparency, В - partial and С- complete cioudness are given in tables. A common picture of activity distribution over year is given in the calendar (Fig.1). The activity levels of three-ball system for every hour of the year are given by the state of the ionosphex'e ( 0 corresponds to ftnir), f £ 3 MIsj 2 - to blackout condition) - upper line, by the geomagnetic field (activity 1 corresponds to 3 0 jsrH $ 1 0 0 ) - middle line and oy auroras (0 - no aurora, 2 - brightness of aurora is not less tnan class 2 or 3 kS) - lower line. The intervals when auroral or ionospheric observations were absent are excluded from the graphs. The days are put in graphs in coluwns according to the Sim's rotations 1934— 1947. The seasonal and daily /ariations of geophysical activity (and sunspot numbers) are given at tfigs 2 and 3 . The activity maximum near midnl, at is connected with the rotation or auroral oval and approaching of Cole peninsula during night hours to che auroral oval. Exept or tne regular variations due to ..he change of position of Earths axis and auroral oval ttie activity undergoes the irregular changes connected with the changes or tne solar corpuscular stream. The examination of magnetograms gives an impression that such variations develop typically as a rather sharp increase of activity f o n o w e d by gradual decrease, un che magnetоgraBf these