Formation of ring-like structures in flared {\alpha}-discs with X-ray/FUV photoevaporation

TL;DR

This study explores how the flaring geometry of protoplanetary discs influences the formation of ring-like structures through photoevaporative winds, using a semi-analytical model to simulate disc evolution.

Contribution

It introduces a combined model of disc flaring and photoevaporative winds to explain ring formation, highlighting the transient nature of these features.

Findings

Flaring geometry can promote ring formation at specific evolutionary stages.

Ring-like features are short-lived in the models.

Further model enhancements are needed for better observational matching.

Abstract

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.