<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>f</mml:mi></mml:math> -mode imprints on gravitational waves from coalescing binaries involving aligned spinning neutron stars

The excitation of $f$-mode in a neutron star member coalescing binaries accelerates the merger course, and thereby introduces phase shift gravitational waveform. Emphasising on tidal by aligned, rotating stars, we provide an accurate, yet economical, method to generate $f$-mode-involved, pre-merger waveforms using realistic spin-modulated frequencies for some viable equations state. We find slow-rotating stars that dephasing effects dynamical tides can be uniquely, EOS-independently determined direct observables (chirp mass ${\cal M}$, symmetric ratio $\eta$ mutual deformability ${\tilde \Lambda}$), while this universality is gradually lost increasing spin. For with fast members ($\gtrsim800\text{ Hz}$) due will exceed uncertainty waveform at reasonable signal-to-noise ($\rho=25$) cutoff frequency $\gtrsim400\text{ Hz}$. Assuming high $10^3\text{ Hz}$ members, significant $\gtrsim100$ rads has been found. systems involving rapidly-spinning (potentially secondary GW190814), neglecting effect templates therefore lead considerable systemic errors relevant analysis. In particular, larger than caused equilibrium factor $\sim5$, which may considerably overestimated if contribution not accounted. possibility accompanying precursors flares also discussed.