  Binary evolution codes are essential tools to help in understanding the
evolution of binary systems. They contain a great deal of physics, for example
stellar evolution, stellar interactions, mass transfer, tides, orbital
evolution. Since many of these processes are difficult to account for in
detail, we often rely on prescriptions obtained in earlier studies. We
highlight that the impact of the dynamical tides with radiative damping has
been implemented inconsistently with respect to its original theoretical
formulation in many studies. We derive a new analytical solution for the
evolution toward synchronization in the case of circular orbits and propose
turnkey equations for the case of eccentric orbits that can be used in
population synthesis studies. We compare the strength of the tidal torque
obtained with this new formula with respect to that obtained with the formula
generally used in literature by studying how the evolution toward
synchronization of main sequence stellar models is affected. We conclude that
by using an incorrect formula for the tidal torque, as has been done in many
binary codes, the strength of the dynamical tides with radiative damping is
over- or underestimated depending on whether the star is close to or far from
synchronization.
