  A theoretical light curve is constructed for the quiescent phase of the
recurrent nova U Scorpii in order to resolve the existing distance discrepancy
between the outbursts (6 kpc) and the quiescences (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, a reflection effect of the MS and the ACDK irradiated
by the WD photosphere. The B light curve is well reproduced by a model of 1.37
M_sun WD + 1.5 M_sun MS (0.8---2.0 M_sun MS is acceptable) with an ACDK having
a flaring-up rim, and the inclination angle i~80 degree. The calculated color
is rather blue (B-V~0.0) for a suggested mass accretion rate of 2.5 x 10^{-7}
M_sun yr^{-1}, thus indicating a large color excess of E(B-V)~0.56 with the
observational color of B-V=0.56 in quiescence. Such a large color excess
corresponds to an absorption of A_V~1.8 and A_B~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 large intrinsic absorption is very consistent
with the recently detected period change of U Sco, which is indicating a mass
outflow of ~3 x 10^{-7} M_sun yr^{-1} through the outer Lagrangian points in
quiescence.
