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Signatures of coupling between an inertial mode in the convective core and agravito-inertial mode in the envelope have been found in four-year Kepler lightcurves of 16 rapidly rotating $\gamma\,$Doradus ($\gamma\,$Dor) stars. Thismakes it possible to obtain a measurement of the rotation frequency in theirconvective core. Despite their similar internal structure and available data,inertial modes have not yet been reported for slowly pulsating B (SPB) stars.We aim to provide a numerical counterpart of the recently published theoreticalexpressions for the mode-coupling coefficients, $\varepsilon$ and$\tilde{\varepsilon}$. These coefficients represent the two cases of acontinuous and a discontinuous Brunt-V\"ais\"al\"a frequency profile at thecore-envelope interface, respectively. We used asteroseismic forward models oftwo samples consisting of 26 SPB stars and 37 $\gamma\,$Dor stars to infertheir numerical values of $\varepsilon$. The asteroseismically inferred valuesof $\varepsilon$ for the two samples are between 0.0 and 0.34. While$\varepsilon$ is most strongly correlated with the near-core rotation frequencyfor $\gamma\,$Dor stars, the fractional radius of the convective core insteadprovides the tightest correlation for SPB stars. We find $\varepsilon$ todecrease mildly as the stars evolve. Our asteroseismic results for the modecoupling support the theoretical interpretation and reveal that young,fast-rotating $\gamma\,$Dor stars are most suitable for undergoing couplingsbetween inertial modes in the rotating convective core and gravito-inertialmodes in the radiative envelope. The phenomenon has been found in 2.4\% of suchpulsators with detected period spacing patterns, whereas it has not been seenin any of the SPB stars so far. (shortened abstract to meet the arXiv limits)

Mode coupling coefficients between the convective core and radiative envelope of $\gamma\,$Doradus and slowly pulsating B stars