  In this paper, we focus on the effect of mass-transfer between compact
binaries like neutron-star-neutron-star (NS-NS) systems and
neutron-star-white-dwarf (NS-WD) systems on gravitational waves (GWs). We adopt
the mass quadrupole formula with 2.5 order Post-Newtonian (2.5 PN)
approximation to calculate the GW radiation and the orbital evolution. After a
reasonable discussion of astrophysical processes concerning our scenario, two
kinds of mass-transfer models are applied here. One is the mass overflow of the
atmosphere, where the companion star orbits into the primary's Roche limit and
its atmosphere overflows into the common envelope. The other one is the tidal
disruption of the core, which is viewed as incompressible fluid towards the
primary star, and in the near region branches into an accretion disc (AD) and
direct accretion flow. Viewing this envelope and as a background, the GW of its
spin can be calculated as a rotating non-spherically symmetric star. We
eventually obtained the corrected gravitational waveform (GWF) templates for
different initial states in the inspiral phase.
