(gk Draconis and V1094 Tauri)

The two stars that form the subject of this paper are both short-period double-lined eclipsing binaries. They have non-circular orbits despite their short periods, both of which are very close to integral numbers of sidereal days (10.0015 and 9.0127 sidereal days respectively), making it difficult to achieve uniform phase coverage of the orbits from a single site in the short term. Although the HD type of HD 152028 is G0, the integrated spectral type of the system must actually be much earlier: the (B − V) colour index is only about 0 m .37 and the Hip-parcos parallax indicates an integrated absolute magnitude as bright as +1 m .4. A published photometric investigation suggests that the primary star exhibits δ Scuti pulsations, with a period of 0.1138 days. That period is not present in the radial velocities, but we have identified a comparable periodicity in the initially excessive residuals (σ ∼ 2 km s –1) in the radial velocities of the primary star: there is an asymmetrical pulsational velocity curve with a semi-amplitude of ∼3 km s –1 and a period of 0.1178 days. The disagreement between that period and the published photometric one is probably because the latter is mistaken. It is argued from the luminosity of the system, the eclipse light-curves in V and (B − V), the lengths of the eclipse chords, and the rotational velocity of the primary star, that the eclipses are practically central (a total eclipse and a transit) and that the component stars have the same colour but luminosities that differ by 1 m .0. HDE 284195 was not observed by Hipparcos, but its HDE type of G0 is in reasonable agreement with its colour and the nature of its radial-velocity traces. The rotations of both stars appear to be pseudo-synchronized to the orbit. Since this is 'only' a radial-velocity study and not a comprehensive discussion of the objects, the orbital inclinations are not formally determined. They must be very high, however (otherwise the systems would not eclipse), and there is specific evidence that the inclination of HD 152028 is very close to 90 • , so it is permissible to assume that the factors sin 3 i in the masses are close to unity. In that case the masses are scarcely above the minimum values, which in the case of HD 152028 are 1.78 and 1.42 M ⊙ and in that of …