Координированные наблюдения авроральных явлений 1-2 декабря и 11-12 декабря 1977 г. на Кольском полуострове и в Финляндии / С. А. Черноус, Н. И. Федорова, Г. А. Логинов и др. ; Акад. наук СССР, Кол. фил. им. С. М. Кирова, Поляр. геофиз. ин-т. – Препр. ПГИ-79-3. - Апатиты : [б. и.], 1979.

south active bands moved eastwards. Between 00.45 and 02.00 bright rayed loops moved over the southern sky from west to east, one after the other. Auroral pulsations followed and continued until 05.00. At 05*04 a red rayed band was seen to travel from west. Red corona formed at 05.10 -05.13 after which pulsating patches were seen until the end of recording at 05.36. Spectral and photometric data. A spectral slit camera was operated in Loparskaya. In M g . 3 we show some examples of the spectral camera recordings on Dec. 1./2. The upper scan was made at 01.30 UT, and shows typical auroral spectra where the green 5577 A (01) emission dominates and the red dublet 6300, 6364 A (01) is weak in intensity. At 04.30 UT, close to the bright red corona,red emission is unusually strong while the 5577 is much weaker than earlier. The I NG inten sities are higher at the later time, when the height of Earth's shadow become less than 350 km. This relatively higher inten sification of I NG wt bands compared to the green line is connected with resonance scattering of sun photons by N^ ions [ 3 ] , which were produced on high altitudes by precipi tating high fluxes of soft electrons. Thus in this event the so called * sunlit aurora" was observed which was described by Stormer [4] . The photographs on the right-hand side of Fig.3 show quite clearly the differences in green and red emissions. In Fig.4 we give data pbtained by spectral camera and by the 70° zenith photometer operated in Loparskaya. The photo meter integrates light over the whole visible spectra with highest sensitivity around 4000 A , which means that the I NG Ng band may dominate in the recordings. The figure tells that on the first night aurora was absent before 18.00 UT. Weak aurora was seen between 18.00 and 20.00 and typical electron aurora was recorded between 20.00 and 03*00 UT. The intensity ratio I 6300/1 5577 equal to 0.1 f 0.3 (see Fig.8 and 10) which was corresponding to energetic spectra of pre cipitating electrons with characteristic energies 10 3 kev, respectively [ 5 ] , After 03.40 UT the red emission dominates ( see Fig.4) and ratio I 6300/1 5577 increases to 3 and in