  Eccentric compact binaries pose not only a challenge for gravitational wave
detectors, but also provide a probe into the nuclear equation of state if one
of the objects is a neutron star. At the short pericenter passage, tidal
interactions excite f-modes on the star, which in turn emit their own
gravitational waves. We derive an analytic waveform for these stellar
oscillations within the effective fly-by framework, modeling the emission to
leading post-Newtonian order. At this order, the f-mode response can be written
in a Fourier decomposition in terms of orbital harmonics, with the amplitudes
of each harmonic depending on Hansen coefficients. Re-summing the harmonics of
the f-mode results in a simple decaying harmonic oscillator, with the amplitude
now determined by a Hansen coefficient of complex harmonic number. We compute
the match ${\cal{M}}$ between the re-summed f-mode and numerical integrations
of the tidal response, and find ${\cal{M}} > 0.97$ for systems with high
orbital eccentriciy $(e > 0.9)$ and low semi-latus rectum $(p < 12 M)$. We
further compare our model to modes generated from multiple pericenter passages
under the effect of radiation reaction, and discuss issues related to the
timing of pericenter passages and its impact on the model.
