  The prime candidate sources for the upcoming space-borne gravitational wave
(GW) observatory LISA are the numerous Galactic tight binaries of white dwarfs
(WDs) and neutron stars (NSs), many of which will coalesce and undergo mass
transfer, leading to simultaneous emission of X-rays and GWs. Here, detailed
and coherent numerical stellar models are explored for the formation and
evolution of these systems, including finite-temperature effects and complete
calculations of mass transfer from a WD to a NS accretor. Evolutionary tracks
of characteristic strain amplitude are computed, and the unique pattern of
their evolution in the GW frequency-dynamical chirp mass parameter space
enables a firm identification of the nature of the systems. Furthermore, it is
demonstrated that a precise detection of the chirp allows determination of the
NS mass to an accuracy of a few per cent, with applications to constraining its
equation-of-state, in particular for dual-line GW sources observed
simultaneously at high and low frequencies.
