In this paper we present the results of some calculations concerning the effects of rotation upon nongray early-type stellar atmospheres. The results consist of forty-six spectral energy distributions for models having various masses, rotational velocities, and angles of inclination. The results are presented in the form of graphs of the monochromatic flux emitted by each model as well as tables of monochromatic magnitudes in units of wavelength and frequency, normalized to X 5048. Additional tables contain the defining values of the models and the numerical value for the monochromatic flux at X 5048. In addition, estimates of UBV colors and absolute magnitude M are given. The models considered include the same models for which H line strengths have been calculated by Collins and Harrington. The variation of the parameters; T and g, which define the local atmosphere structure, is also discussed. The results are critically compared with contemporary work in the field. The possible application of this material to rotational studies of stars in OB associations is considered. It is found that disentanglement of V and V sin i is not possible on the basis of continuum studies alone.
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II Collins George W. (1966) studied this question.