Accretion disk boundary layer models are calculated for the symbiotic
binaries AX Per and CI Cyg, using a time-dependent numerical code. Hot
boundary layers are found with temperatures above 10(5) K, assuming f
or the accreting star a mass M = 0.5 M. and a radius R* = 0.2 R.. How
ever, choosing a larger stellar radius or a smaller stellar mass leads
to cooler boundary layers. The numerical solutions agree fairly well
with the observational estimates of the hot component temperature duri
ng quiescence but do not reproduce the apparent drop in effective temp
erature seen during the outburst of AX Per and CI Cyg. The maximum eff
ective temperature obtained in the boundary layer solutions increases
as the mass accretion rate increases (M = 1-10 x 10(-5) M. yr(-1)) but
then stays nearly constant as the mass accretion rate approaches the
Eddington limit (in the present case, M(Edd) approximate to 10(-4) M.
yr(-1)). In this high accretion rate regime, the disk becomes geometri
cally thick (H/r approximate to 0.4), and the energy dissipated in the
dynamical boundary layer is radiated outward to larger radii and adve
cted into the star. The boundary layer luminosity is only approximate
to 2/3 its expected value; the rest of the energy is advected into the
star.