October 1986 • 1986MNRAS.222..871B
Abstract • The quiescent phase of V2051 Oph is characterized on the basis of photometric observations obtained in H and JHK with the 4.5-m MMT on Apr. 16-17, 1984; in HK with the 3.9-m UKIRT on Apr. 26, 1984; and in UH with the 3.9-m AAT on Apr. 27, 1985. The data and the results of eclipse simulations are presented in extensive tables and graphs and discussed. Nearly sinuosidal optically thin light-curve humps are attributed to disk-temperature (or hotter) material near the white dwarf. These humps (along with superimposed rapid, optically thick, 8000-K flares) are shown to explain most of the gross variability of the accretion-disk eclipses. A model with an optically thin accretion disk and a normal main-sequence red dwarf secondary and an alternative model with an opaque disk and a 2000-K brown dwarf (implying a distance of 110 pc or less) are considered.