  The concept of regular black holes has gained attention in recent years,
especially in the context of quantum gravity theories. In these theories, the
existence of singularities is paradoxical as they represent a breakdown of the
laws of physics. Motivated by the recent developments in this area, we study
the tidal force effects in one such family of regular geometries described by
the Simpson-Visser metric. We find the radial and angular force profiles for a
radially in-falling particle in this spacetime and calculate the variation of
the geodesic separation vector with the radial coordinate using two different
initial conditions. These results are then compared with that of Schwarzschild
black hole spacetime. We show that for a regular black hole, both radial and
angular tidal forces show a peak outside the horizon and then fall to
ultimately switch their behavior from stretching to compression and vice-versa.
Also, they are finite at $r=0$ unlike the Schwarzschild spacetime. It is also
seen that the angular deviation profile shows an oscillating behavior for a
particular initial condition. Our analysis can be used to distinguish between
regular black hole, one-way and two-way wormholes and a singular black hole
spacetimes.
