  In this work, we investigate the influence of planetary tidal interactions on
the transit-timing variations of short-period low-mass rocky exoplanets. For
such purpose, we employ the recently-developed creep tide theory to compute
tidally-induced TTVs. We implement the creep tide in the recently-developed
Posidonius N-body code, thus allowing for a high-precision evolution of the
coupled spin-orbit dynamics of planetary systems. As a working example for the
analyses of tidally-induced TTVs, we apply our version of the code to the
K2-265 b planet. We analyse the dependence of tidally-induced TTVs with the
planetary rotation rate, uniform viscosity coefficient and eccentricity. Our
results show that the tidally-induced TTVs are more significant in the case
where the planet is trapped in non-synchronous spin-orbit resonances, in
particular the 3/2 and 2/1 spin-orbit resonant states. An analysis of the TTVs
induced separately by apsidal precession and tidally-induced orbital decay has
allowed for the conclusion that the latter effect is much more efficient at
causing high-amplitude TTVs than the former effect by 2 - 3 orders of
magnitude. We compare our findings for the tidally-induced TTVs obtained with
Posidonius with analytical formulations for the transit timings used in
previous works, and verified that the results for the TTVs coming from
Posidonius are in excellent agreement with the analytical formulations. These
results show that the new version of Posidonius containing the creep tide
theory implementation can be used to study more complex cases in the future.
For instance, the code can be used to study multiplanetary systems, in which
case planet-planet gravitational perturbations must be taken into account
additionally to tidal interactions to obtain the TTVs.
