Venusian "hot spots": physical phenomenon and its quantification.
An overall picture of the Venusian hot spots phenomenon is considered in the framework of the simplest conceptual models that admit the solutions in the form of steadily rotating "hot" vortices. Model assumptions take into account only those features of the middle atmosphere in the polar region of Venus that are supported by observational data and are essential for understanding the physical mechanism initiating similar vortices. The problem is analyzed in the framework of both the pointlike and petal-like models of cyclostrophic vortices. Interpretation of these models as an upper and lower bound of a complete theory allows one to find the region of existence of the regimes responsible for the Venusian hot spots and also to establish and assess numerically conditions under which such vortices can be formed. The emphasis is on a comparison of the theoretically established results with the observational data.