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Flare colours determined from simultaneous UBV observations made at Catania Observatory and from sequential UBV observations made at McDonald Observatory are presented. They fit fairly well with the theoretical colours computed according to the Gurzadian's (1970) non-thermal model. Only part of the observed flare colours are consistent with the solar type models by Gershberg (1967) and Kunkel (1970).From a B-band patrol of UV Cet-type stars carried out from 1967 to 1972, some quantitative estimates of flare frequencies and luminosities and of their average contribution to the stellar radiation are given.The corresponding parameters for the Sun, which were estimated from ‘white light’ flare activity, are also given for comparison. The Sun and V 1216 Sgr can be regarded as low-activity flare stars of the type found by Kunkel (1973).

Es werdcn 157 lichtclektrische Messungen des kurzperiodischen Algolveranderlichcn AT Pegasi mitgetcilt, aus dcnen die Lichtkurve und die relativen Dimensionen des Systems abgeleitet werden.Der Bedeckungsveranderliche AT Pegasi [a = zh I I ' ?~, 6 = +8" 13 ' (1961)