1. Introduction

The variability of V 700 Cyg (Oklahoma Variable 26) was discovered by Whitney (1952), who classified it as a W UMa system with a period of 0.340048 days. Besides the minima given by Whitney, photographic ones were published by Busch et al. (1964) and Romano (1969), photoelectric ones by Hoffmann (1983) and by members of the BAV (Agerer & Hübscher 1995). Visual minima were observed by members of the BBSAG (Bulletins 23, 25, 39, 49, 50, 51 and 56).

Eggen (1967) noted the presence of a close physical companion and derived the following magnitudes and colours:

 t#tex2html_wrap_inline1682#Ī<>B-VĪ<>U-BĪ<>E(B-V)

V 700 Cyg   		 11.2 		  +0.74 		 +0.14 		 +0.03

Companion  		 12.59		 +0.88 		+0.45.

Its spectral type was determined to be F2 from objective prism spectra taken with the 10-inch Cooke refractor of the Leander McCormick Observatory (MacDonald 1964). Götz & Wenzel (1967) derive a spectral type of A from Sonneberg Schmidt plates. Eggen's colours, however, indicate a much later spectral type. Since a good temperature estimate is essential for the analysis, Wenxian Lu (U. of Toronto) kindly took a CCD spectrum of V 700 Cyg, covering the range , with the Cassegrain spectrograph of the David Dunlap Observatory 1.9m telescope. It was compared with main sequence star spectra from the atlas of Yamashita et al. (1977). The spectral type was found to be G5, in good agreement with the UBV colours. The cause of the discrepancy of the old classifications is not clear; maybe the presence of the nearby visual companion has influenced the appearance of the spectrum of V 700 Cyg on the objective prism plates.

The variability of AW Vir was discovered by Hoffmeister (1935) on Babelsberg and Sonneberg plates. He found short-time light variability and suspected it to be an eclipsing binary. This was confirmed by Jensch (1936) who gave a list of minimum times, based on photographic and visual observations, and derived an ephemeris. Further minima were reported by Whitney (1955), Koch (1961), Hoffmann (1983), Lapasset & Gómez (1995), and by members of the BBSAG (Bulletins 48, 67, 83, 88, 89, 92, 95, 97, 98, 101, 104, 109; visual and CCD). Its spectral type was determined on objective prism spectra as F8 (MacDonald 1964). A synthetic light curve analysis of AW Vir was recently presented by Lapasset et al. (1996), who analysed B and V light curves collected in 1989.