Institute Physics of Earth, Academy of Sciences of the USSR H,0 and OH maser sources are observed in the direction of compact regions of HII and IR stars and molecular complexes. Besides,the maser sources are observed in the direction of star formation regions and are associated with Herbiga-Aro objects and T-Tau stars.The list of the observed objects, with which in any case H O and OH masers are associated, demonstrates that the maser phenomenon accompanies as the star formation as exists in the process of its evolution. H,0 and OH maser sources observed in the direction of compact HII regions and IR stars apparently are clouds formed as a result of thermal instability after the shock wave passage (Burdjuzha, Ruzmaikina 1974). The shock waves are generated either by a stellar wind or are formed before the ionization front of D-type. The maser clouds where the temperature is lower and the density is higher than in the environment, are in hydrostatic equilibrium with it. Usually they are localized to the periphery and near the HII compact region or in the IR-star envelope and are at about 10 -r 10 cm from the central star. The cloud masses are about 1 0 " + l O " g. The estimates of OH and H O maser cloud mass were obtained from the observed luminosities of maser sources and probable pumping rate with normal concentration of elements and also from their visible dimensions and restrictions on the density. Such masses of the maser clouds suggest an idea that during cooling the maser sources can change either into protoplanets or into comets. The papers (Strelnitsky et al. 1972, Oppenheimer 1975 took notice of the evolutionary connection between the maser sources, the protoplanets and the comets.H-0 thermal balance of the maser regions (as the hottest and the brightest) in the sources connected with HII compact regions and IR stars was analysed. There are two different regions with maser properties :terms of use, available at https://www.cambridge.org/core/terms. https://doi
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