A new 3D hydrodynamical tree-based code for the investigation of the evolution of circumbinary radiative self-gravitating gaseous disks.

At present, the study of the evolution of matter around young binary systems is a key issue which can provide important answers on the possibility of forming planets in stable orbits around two stars. In the context of my PhD work in Astronomy, Astrophysics and Space Science, me and my research group aim at studying the conditions for stability of gaseous disks revolving around binary stars, during the earliest phases of planet formation, when no km-sized planetesimal has been constituted yet and the circumbinary matter is still made up of just gas and dust. The stability of such systems, maintained for a sufficiently large time-scale, will be a crucial condition for matter condensation and for the following planet constitution. For this purpose, we intend to perform several 3D high resolution simulations by implementing a Smoothed Particle Hydrodynamics tree-based code, suitably designed to take efficiently into account both the selfgravity of the system and the influence of the stellar radiation. Previously, few works focused their attention to this problem and, to overcome several issues due to computational efforts, some approximations have been used. Despite important constraints for the regions of stability have been obtained, no characterization in high details on the structure of the disk nor clear informations about its symmetry have been given. By contrast, our code will be realized to take into account several physical processes, relevant for disk stability, exploiting some suitable numerical techniques previously developed by several authors. In particular, self-gravity and stellar radiation absorption, which in many cases have been considered in a simplified theoretical scheme, are thought to play a crucial role. Our algorithm is designed to be flexible, due to its lagrangian structure, and efficient, since it will run in multi-node architectures. Such poster shows a preliminary part of our work which consists in the realization of a serial version of the code, able to simulate the hydrodynamical evolution of a gas system which interacts gravitationally with two stars (represented by point mass objects)