  One of the important targets for the future space-based gravitational wave
observatory LISA is extreme mass ratio inspirals (EMRIs), where long and
accurate waveform modeling is necessary for detection and characterization.
Modeling EMRI dynamics requires accounting for effects such as the ones induced
by an external tidal field, which can break integrability at resonances and
cause significant dephasing. In this paper, we use a Newtonian analogue of a
Kerr black hole to study the effect of an external tidal field on the dynamics
and the gravitational waveform. We have developed a numerical framework that
takes advantage of the integrability of the background system to evolve it with
a symplectic splitting integrator, and compute approximate gravitational
waveforms to estimate the timescale over which the perturbation affects the
dynamics. Comparing this timescale with the characteristic time under radiation
reaction at resonance, we introduce a tool for quantifying the regime in which
tidal effects might be included when modeling EMRI gravitational waves. As an
application of this framework, we perform a detailed analysis of the dynamics
at one resonance to show how different entry points into the resonance in
phase-space can produce substantially different dynamics, and how one can
estimate bounds for the parameter space where tidal effects may become
dominant. Such bounds will scale as $\varepsilon \gtrsim C \, q$, where
$\varepsilon$ measures the strength of the external tidal field, $q$ is the
mass ratio, and $C$ is a number which depends on the resonance and the shape of
the tide. We demonstrate how to estimate $C$ using our framework for the 2:3
radial to polar frequency resonance in our model system. This framework can
serve as a proxy for proper modeling of the tidal perturbation in the fully
relativistic case.
