  Tidally excited oscillations (TEOs) in Heartbeat Stars (HBSs) are an
essential probe of the internal properties of the systems, but their potential
has yet to be fully exploited. Based on the orbital parameters of TEO
candidates from our previous works, we identify the pulsation phases and
amplitudes of TEOs in fourteen Kepler HBSs. Most pulsation phases of most
systems can be explained by the dominant being $l=2$, $m=0$, or $\pm2$
spherical harmonic, assuming that the spin and orbital axes are aligned, and
the pulsations are adiabatic and standing waves. The largest deviation
($>6\sigma$) occurs in KIC 8459354, which can be explained by the spin-orbit
misalignment, and KIC 5877364 has a similar scenario. For KIC 11122789, almost
half of the harmonics show large deviations; we cautiously suggest that these
harmonics may not be considered TEO candidates. A similar scenario also exists
in KIC 6290740. This phases and mode identification approach can also be used
inversely to verify the TEO candidates derived by the Fourier analysis.
Furthermore, the harmonics with large deviations ($>2\sigma$) in KIC 4377638,
KIC 5090937, and KIC 11403032 can be expected to be travelling waves rather
than standing waves. In addition, we also suggest that the apsidal motion could
cause large deviations in TEO phases from theoretical values.
