Single-trail spectra of SX Phe have been obtained covering many cycles of this short-period dwarfcepheid variable at a dispersion of 18 Å mm⁻¹. The rapid changes in line intensities and the line doubling reported by Stock and Tapia (1971a) from 40 Å mm⁻¹ plates are not evident in our spectra.

Photometric (uvbyfi) observations of the RRc variable SS Psc suggest that it is more closely related to dwarf cepheids (RRs stars) than to the RRc variables. Intrinsic (b — y) and c₁ values are employed to derive the variations in surface gravity and temperature. The mean values are (log g eff) = 3.29 and (T eff ) = 7300° K. The mi index, ((mi) 0 ) = 0.178, and spectrum indicate it is a metal-strong star.

The geometric and photometric elements of the eclipsing star U Sge have been derived from uvby observations secured in 1973-74. The "best" elements are r₁ = 0.296, r₂ = 0.225, i = 90°; and L₁ = 0.130, L₂ = 0.870 in yellow light where the subscript 1 refers to the G2 IV-III component and the subscript 2 refers to the B8 V component. Radii and masses of the two stars can be derived by assuming that the larger star fills its Roche lobe. This assumption yields r₁ = 3.32 R⊙, r₂ = 2.52 ⊙, 𝕸₁ = 1.4⊙, and 𝕸₁ = 3.5⊙. The absolute magnitudes are found by two different methods and yield Mv = —0ṃ4 for the B star and Mv = +1ṃ8 for the G star. If corrections for radiative interactions are made, the absolute magnitude of the G star is Mv ≃+2ṃ2. Observational data secured in the u filter suggest that Balmer continuum emission can be detected from an emitting gas stream or disk. The gas must be concentrated near the following hemisphere of the B Star. The mi measurements of the secondary component suggest a metal deficiency of [Fe/H] = —0.6.

Photometric (uvbyβ) and spectrographic observations of the dwarf cepheid RS Gru are described. The photometry suggests that the star is slightly reddened, E(b-y)=+ 0ṃ026. Intrinsic (b-y) and c values are used to derive the variations in temperature and surface gravity. The mean values are >Teff< = 7620° and (log geff) = 3.83. With the aid of Wesselink's method, a radius of 3.1 Rṃ is found. The radius and effective temperature indicate Mv = + 1.2 which agrees well with the value Mv = + 1.3 derived directly from the photometry. A mass of 2.4 � � is found from the radius and effective gravity. The radial-velocity data indicate that γ = 82 km sec¹ and 2K = 49 km sec¹.

Photometric observations of RZ Set in the (U, B, and V passbands are described. Because of distortions in the light curves it is difficult to derive accurate light elements. The "best" light elements are r₁ = 0.26, r₂ = 0.26, k = 1, i = 84°, and L = 0.89, L₂ = 0.11 in yellow light. At fourth contact the system is approximately 0ṃ1 brighter than at first contact. The decrease in light near first contact is attributed to Thompson scattering by free electrons in circumstellar material. Estimates of the spectral types and absolute magnitudes of the two stars yield B2 (-4ṃ6) and A0(-2ṃ3). Both stars have radii ~ 14 R⨀ and are = 2ṃ5 brighter than main-sequence stars of similar spectral types. It appears that the secondary star fills its Roche limit. The color excess of the system is E(B–V) $ \simeq $ 0ṃ86.