Energy Distribution in the Spectra of Early-Type Stars.

Application of Spectrophotometry to a Binary Star Problem

“…To do this we adjust the ratio of flux scale factors for the two components until we reproduce the observed composite spectral distribution. Since a reasonably large number of single stars have now been observed spectrophotometrically by Bahner (1963), Oke (1960Oke ( , 1964Oke ( , 1965, Wilstrop (1965) and others*, we do know, to adequate accuracy, the spectral distribution of any star for which we know the spectral type, although correction for interstellar reddening may sometimes be necessaiy. Of course the spectral types of the components must be different, probably by a least two classes, and the best results will be found when a crossover point in wavelength from L g > L s to L s > L g occurs near the middle of the observed range.…”