  The energy dissipation of wave-like tidal flows in the convective envelope of
low-mass stars is one of the key physical mechanisms that shape the orbital and
rotational dynamics of short-period planetary systems. Tidal flows, and the
excitation, propagation, and dissipation of tidally-induced inertial waves can
be modified by stellar magnetic fields (e.g., Wei 2016, 2018, Lin and Ogilvie
2018). It is thus important to assess for which stars, at which location of
their internal structure, and at which phase of their evolution, one needs to
take into account the effects of magnetic fields on tidal waves. Using scaling
laws that provide the amplitude of dynamo-generated magnetic fields along the
rotational evolution of these stars (e.g., Christensen et al. 2009, Brun et al.
2015), combined with detailed grids of stellar rotation models (e.g., Amard et
al. 2016), we examine the influence of a magnetic field on tidal forcing and
dissipation near the tachocline of solar-like stars. We show that full
consideration of magnetic fields is required to compute tidal dissipation, but
not necessarily for tidal forcing.
