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In an earlier investigation, we proposed population boundaries for bothinspiralling and mass-transferring double white dwarf (DWD) systems in thedistance independent "absolute" amplitude-frequency domain of the proposedspace-based gravitational-wave (GW) detector, {\it LISA}. The degenerate zerotemperature mass-radius (M-R) relationship of individual white dwarf stars thatwe assumed, in combination with the constraints imposed by Roche geometries,permits us to identify five key population boundaries for DWD systems invarious phases of evolution. Here we use the non-zero entropy donor M-Rrelations of \cite{DB2003} to modify these boundaries for both DWD and neutronstar-white dwarf (NSWD) binary systems. We find that the mass-transferringsystems occupy a larger fraction of space in ``absolute'' amplitude-frequencydomain compared to the simpler T=0 donor model. We also discuss how theseboundaries are modified with the new evolutionary phases found by\cite{Deloyeetal2007}. In the initial contact phase, we find that the contactboundaries, which are the result of end of inspiral evolution, would have somewidth, as opposed to an abrupt cut-off described in our earlier T=0 model. Thiswill 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 donorevolution, the radius contracts, mass-transfer rate drops and slows down theorbital period evolution. Depending upon the entropy of the donor, thesesystems may then lie inside the fully degenerate T=0 boundaries, but LISA maybe unable to detect these systems as they might be below the sensitivity limitor within the unresolved DWD background noise.

Population boundaries for compact white-dwarf binaries in LISA's amplitude-frequency domain