The intensive patrol observations of red dwarf stars during last years, carried out in the Crimea, Chile, Catania, South Africa, Armenia, Japan and other observatories led to appreciable increase of number of known UV Ceti-type objects. It permits us to complete the known lists of the variables (1—4). At the same time it is worth-while to define more precisely the criteria to consider a star as the UV Ceti-type variable, and to carry out strong selection of the certain UV Cet-type variables from the objects suspected to be this type variables.