  Massive and intermediate-mass stars reside in binary systems much more
frequently than low-mass stars. Binaries containing massive main-sequence (MS)
component(s) are often characterised by eccentric orbits, and can be observed
as eccentric ellipsoidal variables (EEVs). The orbital phase-dependent tidal
potential acting on the components of EEV can induce tidally excited
oscillations (TEOs). We investigate how the history of resonances between the
eigenmode spectra of the EEV components and the tidal forcing frequencies
depends on the initial parameters of the system. We synthesised 20,000
evolutionary models of the EEVs across the MS. Later, we calculated the
eigenfrequencies for each model. We focused only on the $l=2$, $m=0,+2$ modes.
Knowing the temporal changes in the orbital parameters of simulated EEVs and
the changes of the eigenfrequency spectra for both components, we were able to
determine so-called `resonance curves', which describe the overall chance of a
resonance occurring. We analysed the resonance curves by constructing basic
statistics for them and analysing their morphology using machine learning
methods, including the Uniform Manifold Approximation and Projection tool. The
EEV resonance curves from our sample are characterised by striking diversity,
including the occurrence of exceptionally long resonances or the absence of
resonances for long evolutionary times. Both components may be subject to
increased resonance rates as they approach the TAMS. On average, we should
observe TEOs more frequently in EEVs containing massive components than
intermediate-mass ones. TEOs will be particularly well-pronounced for EEVs with
the component(s) close to the TAMS. Given the total number of resonances and
their rates, TEOs may play an important role in the transport of angular
momentum within massive and intermediate-mass stars (mainly near TAMS).
