Аскаплоты советских станций за 1984 год : (оперативно-информационный материал) / Акад. наук СССР, Кол. фил. им. С. М. Кирова, Поляр. геофиз. ин-т. – Апатиты : Кольский филиал АН СССР, 1990.

II Soviet asoafilms equals to the order of two. Each film baa a4standard sensitive wedge made by an i'SR~4 sansitometer»» All the negatives from the stations enumerated in Sable 1 are kept in the Auroral Subcenter of the World Data Centra WDC B2 located in Apatity (eddreesz Auroral Subcontxe* Volar Geophysical Institute, Kola 'Science Centre of the USSR Academy of Sciences, 184200 Apatity Murmansk i*egion, USSR). Methods of aaoaplotting. Information about auroras for every station", according to /1,2/ is encoded in 5 lines divided by vertical linos?» One vertical dividing corresponds to a half-an-hour interval centered to tha beginning and the middle of each hour (UT). The local geomagnetic midnight is marked by a circle under the ascaplot. l’bree upper lines show aurora location in the sky. She upper blackened line demonstrates that in a given half-an-hour interval auroras were observed within the scale of the zenith angle from 60 ° to 80° N. The second blackaned line corresponds to auroras in th® zenith (from 60° N to 60° S) and the third one shows auroras in the south (from 60° to 80° S). Ocourenc® of aurora a in the corresponding part of the sky was marked when an aurora was observed during a single minute in a given time interval. Tha auroral location waa defined by its bottom edge. Suppose that the height of the lower edge is equal to 100 km then we gat that all three zenith angle intervals have approzimstely sufficient extent along thw meridian corresponding to 3 degrees of latitude. Thus, ascaplota give information on spatial distribution of auroras in 9“degree~latitude range with its centre in the zenith of the station. It should be taken into account that the sensitivity of all-sky cameras is maximum for the zenith and it diminishes when the zenith angle increases, i.e„ to the frame edge. The presence of stars on the films makes it possible to judge on meteo~ rological conditions in every latitude interval. According to /1,2/ the dot in the middle of the square shows weak cloudiness or cloudiness with rents in the given part of the sky and in the given time-interval. The vertical line denotes complete cloudiness. The tick inside the square of the third line points to a bad quality of the ascafilm caused by some technical reasons (inaccurate focusing, poor quality of development etc.). The horizontal line denotes that no observations were carried out. To mark moon lightening which sufficiently reduces the quality of asoafilms we used an additional designation, i.e. the horizontal line over the ascaplot. Two bottom lines of squares carry tha information about auroral activity. Blackening of tha very bottom line means that 2 ball aurora was observed» Blackening of the two bottom lines refers to 3 ball auroral activ ity. It should be noted that the activity in ascaplots does not entirely coincide with brightness of forras, The ball of activity also includes such parameters as type of the form and its life-time within the given half-an- hour interval. Since the compresion of the angle range for the north and the south does not permit similar determinations of peculiarities of auroral forms, the auroral activity in ascaplota was estimated only for tha aenith region. The series of auroral activity, which was offered in /7/, characteriz ing the connection between the substorm phase and substorm intensity on one hand , and the type of the form on the other, was taken aa a basis. The table for estimating the activity is given in i4gure 1. Here the balls of activity are marked at the bottom, horizontal lines denote the types of