  According to core-accretion formation models, the conditions under which gas
giants will form around M dwarfs are very restrictive. Also, the correlation of
the occurrence of these planets with the metallicity of host stars is still
unknown due to the intrinsic faintness of M dwarfs in the optical and some
intricacies in their spectra. Interestingly, NASA's TESS mission has started to
create a growing sample of these systems, with eleven observed planets located
in close-in orbits: contrary to what is expected for low stellar masses. Tidal
interactions with the host star will play a key role in determining the fate of
these planets, so by using the measured physical and orbital characteristics of
these M-dwarf systems we numerically analyse the exchange of rotational and
orbital angular momentum, while constraining the energy dissipation in each
system to calculate whether host stars are spun up or spun down, depending on
the relationship between the gain and loss of angular momentum by the stellar
rotation. We also study the coupled orbital and physical evolution of their gas
giant companion and calculate orbital circularization time-scales, as well as
the time needed to undergo orbital decay from their current orbital position to
the Roche limit. The thorough study of tidal processes occurring over short and
long time-scales in star-planet systems like those studied here, can help
constrain tidal dissipation rates inside the star and planet, complement tidal
theories, and improve estimations of unconstrained properties of exoplanetary
systems.

Earth and Planetary Astrophysics;Solar and Stellar Astrophysics