Effective temperatures, angular diameters, distances and linear radii for 160 O and B stars

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Abstract
The significance of the effective temperatures, angular diameters, distances and linear diameters which we have found from published ultraviolet spectrophotometry, visible and near infrared intermediate-band photometry and model-atmosphere fluxes for 160 O and B stars using a method which is fully explained and evaluated in the full paper which is reproduced on Microfiche MN 189/1 is discussed here. An appendix to our full paper presents BCD spectrophotometry for 77 of the program stars. Our angular diameters are systematically the same as those measured by Hanbury Brown et al. and the flux effective temperatures of the main-sequence and giant stars reproduce well the relationship established by Code et al. for mainsequence and giant O and B stars. The 08–B9 supergiants have systematically lower temperatures than do main-sequence stars of the same subtype. The Beta Cephei stars and most Be stars have the same effective temperature as normal stars of the same spectral type. The radii of O and B stars increase from main-sequence to supergiant. The late B supergiants are about twice as large as the O9 supergiants.

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