A model for the quiescent phase of the recurrent nova U Scorpii

A theoretical light curve is constructed for the quiescent phase of the rec urrent nova U Scorpii in order to resolve the existing distance discrepancy between the outbursts (d similar to 6 kpc) and the quiescences (d similar to 14 kpc). Our U Sco model consists of a very massive white dwarf (WD), an accretion disk (ACDK) with a flaring-up rim, and a lobe-filling, slightly evolved, main-sequence star (MS). The model properly includes an accretion luminosity of the WD, a viscous luminosity of the ACDK, and a reflection ef fect of the MS and the ACDK irradiated by the WD photosphere. The B light c urve is well reproduced by a model of 1.37 M. WD + 1.5 M. MS (0.8-2.0 M. MS is acceptable) with an ACDK having a flaring-up rim and the inclination an gle of the orbit i similar to 80 degrees. The calculated color is rather bl ue (B-V similar to 0.0) for a suggested mass accretion rate of 2.5 x 10(-7) M. yr(-1) thus indicating a large color excess of E(B-V) similar to 0.56 w ith the observational color of B-V = 0.56 in quiescence. Such a large color excess corresponds to an absorption of A(V) similar to 1.8 and A(B) simila r to 2.3, which reduces the distance to 6-8 kpc. This is in good agreement with the distance estimation of 4-6 kpc for the latest outburst. Such a lar ge intrinsic absorption is very consistent with the recently detected perio d change of U Sco, which is indicating a mass outflow of similar to 3 x 10( -7) M. yr(-1) through the outer Lagrangian points in quiescence.