  In an earlier investigation, we proposed population boundaries for both
inspiralling and mass-transferring double white dwarf (DWD) systems in the
distance independent "absolute" amplitude-frequency domain of the proposed
space-based gravitational-wave (GW) detector, {\it LISA}. The degenerate zero
temperature mass-radius (M-R) relationship of individual white dwarf stars that
we assumed, in combination with the constraints imposed by Roche geometries,
permits us to identify five key population boundaries for DWD systems in
various phases of evolution. Here we use the non-zero entropy donor M-R
relations of \cite{DB2003} to modify these boundaries for both DWD and neutron
star-white dwarf (NSWD) binary systems. We find that the mass-transferring
systems occupy a larger fraction of space in ``absolute'' amplitude-frequency
domain compared to the simpler T=0 donor model. We also discuss how these
boundaries are modified with the new evolutionary phases found by
\cite{Deloyeetal2007}. In the initial contact phase, we find that the contact
boundaries, which are the result of end of inspiral evolution, would have some
width, as opposed to an abrupt cut-off described in our earlier T=0 model. This
will cause an overlap between a DWDs $&$ NSWDs evolutionary trajectories,
making them indistinguishable with only LISA observations within this region.
In the cooling phase of the donor, which follows after the adiabatic donor
evolution, the radius contracts, mass-transfer rate drops and slows down the
orbital period evolution. Depending upon the entropy of the donor, these
systems may then lie inside the fully degenerate T=0 boundaries, but LISA may
be unable to detect these systems as they might be below the sensitivity limit
or within the unresolved DWD background noise.
