  Recent observational results show that very low mass stars and brown dwarfs
are able to host close-in rocky planets. Low-mass stars are the most abundant
stars in the Galaxy and the formation efficiency of their planetary systems is
relevant in the computation of a global probability of finding Earth-like
planets inside habitable zones. Tidal forces and relativistic effects are
relevant in the latest dynamical evolution of planets around low-mass stars and
their effect on the planetary formation efficiency still needs to be addressed.
Our goal is to evaluate the impact of tidal forces and relativistic effects on
the formation of rocky planets around a star close to the substellar mass
limit, in terms of the resulting planetary architectures and its distribution
according to the corresponding evolving habitable zone. Thus, we performed a
set of $N$-body simulations spanning the first 100~Myr of the evolution of two
systems composed respectively by 224 embryos with a total mass 0.25M$_\oplus$
and 74 embryos with a total mass 3 M$_\oplus$ around a central object of
0.08~M$_\odot$. For these two scenarios, we compared the planetary
architectures that result from simulations that are purely gravitational with
those from simulations that include the early contraction and spin-up of the
central object, the distortions and dissipation tidal terms and general
relativistic effects. We found that including these effects allows the
formation and survival of a close-in population located in the habitable zone
of the system. This means that both effects are relevant during the formation
of rocky planets and their early evolution around stars close to the substellar
mass limit, in particular when low-mass planetary embryos are involved.
