Gravitational wave forms of galactic compact binaries with mass-transfer correction

In this paper, we focus on the effect of mass-transfer between compact binaries like neutron star--neutron star systems and neutron star--white dwarf systems on gravitational waves (GWs). We adopt the mass quadrupole formula with 2.5 order post-Newtonian 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 disk and direct accretion flow. Viewing this envelope and as a background, the GW of its spin can be calculated as a rotating nonspherically symmetric star. We eventually obtain the corrected gravitational waveform templates for different initial states in the inspiral phase.