  We find the central stars of the planetary nebulae (PNe) HaTr 7 and ESO 330-9
to be close binary systems. Both have orbital periods of less than half a day
and contain an irradiated cool companion to the hot central star. We provide
light curves, spectra, radial velocity curves, orbital periods, and binary
modeling results for both systems. The binary modeling leads to system
parameters, or ranges of allowed parameters for each system. We find that for
the CS of HaTr 7 we need to use limb-darkening values for the cool companion
that are different than the expected values for an isolated star. We also fit
the central star spectrum to determine $\log g$ and temperature values
independent of the binary modeling. For ESO 330-9 we find that based on our
binary modeling the hot central star is most likely a post-RGB star with a mass
of around 0.4 M$_\odot$. We discuss our derived stellar and nebular parameters
in the broader context of close binary central stars and their surrounding PNe.
We also discuss the present status of known or suspected post-RGB stars in PNe.
