  Protoplanetary discs are complex dynamical systems where several processes
may lead to the formation of ring-like structures and planets. These discs are
flared following a profile where the vertical scale height increases with
radius. In this work, we investigate the role of this disc flaring geometry on
the formation of rings and holes. We combine a flattening law change with X-ray
and FUV photoevaporative winds. We have used a semi-analytical 1D viscous
{\alpha} approach, presenting the evolution of the disc mass and mass rate in a
grid of representative systems. Our results show that changing the profile of
the flared disc may favour the formation of ring-like features resembling those
observed in real systems at the proper evolutionary times, with proper disc
masses and accretion rate values. However, these features seem to be
short-lived and further enhancements are still needed for better matching all
the features seen in real systems.
