  Tidal effects in gravitational-wave (GW) observations from binary neutron
star mergers have the potential to probe ultra-dense matter and shed light on
the unknown nuclear equation of state of neutron stars. Tidal effects in
inspiralling neutron star binaries become relevant at GW frequencies of a few
hundred Hz and require detectors with exquisite high-frequency sensitivity.
Third generation GW detectors such as the Einstein Telescope or Cosmic Explorer
will be particularly sensitive in this high-frequency regime, allowing us to
probe neutron star tides beyond the adiabatic approximation. Here we assess
whether dynamical tides can be measured from a neutron star inspiral. We find
that the measurability of dynamical tides depends strongly on the neutron star
mass and equation of state. For a semi-realistic population of 10,000
inspiralling binary neutron stars, we conservatively estimate that on average
$\mathcal{O}(50)$ binaries will have measurable dynamical tides. As dynamical
tides are characterised not only by the star's tidal deformability but also by
its fundamental ($f$-) mode frequency, they present a possibility of probing
higher-order tidal effects and test consistency with quasi-universal relations.
For a GW170817-like signal in a third generation detector network, we find that
the stars' $f$-mode frequencies can be measured to within a few hundred Hz.
