  Gravitational waves from inspiralling binary neutron stars provide unique
access to ultra-dense nuclear matter and offer the ability to constrain the
currently unknown neutron star equation-of-state through tidal measurements.
This, however, requires the availability of accurate and efficient tidal
waveform models. In this paper we present PhenomGSF, a new phenomenological
tidal phase model for the inspiral of neutron stars in the frequency-domain,
which captures the gravitational self-force informed tidal contributions of the
time-domain effective-one-body model TEOBResumS. PhenomGSF is highly faithful
and computationally efficient, and by choosing a modular approach, it can be
used in conjunction with any frequency-domain binary black hole waveform model
to generate the complete phase for a binary neutron star inspiral. PhenomGSF is
valid for neutron star binaries with unequal masses and mass ratios between 1
and 3, and dimensionless tidal deformabilities up to 5000. Furthermore,
PhenomGSF does not assume universal relations or parameterised
equations-of-state, hence allowing for exotic matter analyses and beyond
standard model physics investigations. We demonstrate the efficacy and accuracy
of our model through comparisons against TEOBResumS, numerical relativity
waveforms and full Bayesian inference, including a reanalysis of the binary
neutron star observation GW170817.
