Abstract
Einstein and IUE observations on main sequence close binaries are fitted with approximate power-laws of type F ∝ Ωαfβ where Ω is the angular velocity (period-1) and f the convective efficiency (∼ Teff-7). The data suggest the reducing nature of binarity for the X- and UV-activity (tidal effects, mass and energy transfer in contact binaries). The whole surface of the most active stars can be visualized to be entirely filled with structures similar to those found in strong solar active regions. The results are roughly compatible with the constancy of the differential emission measure between 105 K and Tmax in static loop-models. The total radiative losses from the upper atmosphere may be simply proportional to the angular velocity, in spite of different Ω-dependences in separate wavelength-bands. The peculiar behaviour of physical-contact binaries of W UMa-type is remarked upon.
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