  We used the light curve code XRBinary to model the quiescent K2 light curves
of three low-inclination cataclysmic variables (CVs): 1RXS\,J0632+2536
(J0632+2536), RZ\,Leo, TW\,Vir and the pre-CV WD\,1144+011. Optimized light
curve models were obtained using a nonlinear fitting code NMfit and visualized
by Phoebe 2.0. The disk model of J0632+2536 shows that one hotspot at the edge
of the disk is enough to describe its light curve, while the other two dwarf
nova (DN): RZ\,Leo and TW\,Vir require two hotspots. A typical pre-CV model
with a weak irradiation effect for WD\,1144+011 can explain its single-hump
modulation, and the newly observed spectrum confirms its previous
classification. The synthetic analyses for the DN clearly indicate that phase
zero of the double-hump modulations occurs around the secondary minimum and the
primary hump is mainly caused by the hotspot at the edge of the disk. The
quiescent disk has a flat temperature distribution with a power index of
$\sim0.11$. The disk model of RZ\,Leo implies a truncated disk, supporting its
previously speculated classification as an intermediate polar (IP). Except for
the IP model of RZ\,Leo, which lacks a component related to the inferred
accretion curtain, the models of J0632+2536, TW\,Vir and WD\,1144+011 are
consistent with results from the Gaia mission. The derived masses and radii of
the secondaries of the three DN are consistent with the semi-empirical
relations for CV donor stars, while their effective temperatures are higher
than the predictions. Irradiation of the donor stars is investigated to explain
this discrepancy.
