The Solar System dynamical interaction with the Galaxy environment: evolutionary implications for alien Oort clouds and exo-planets

The Sun is located in the Orion Arm of the Milky Way galaxy and its surrounded, along with other bodies, by stars. This thesis work aims at understanding whether these stars can dynamically interact with the Sun and its Solar System and to investigate the possible features of this kind of interactions. We will begin from an observable quantity, the Oort surface density for stars, and we will build a stellar density profile for the Milky Way galaxy using the model suggested by Juric et al., 2008. Then, making use of the Initial Mass Function and the Star Formation Rate function, we will calculate the Present Day Mass Function to have the correct distribution of mass along stellar classes. From kinematic concepts such as the rotation curve, the Oort constants, and the Local Standard of Rest we will characterize the motion of the Sun in the Galaxy, assuming for our calculations a value v=14 km/s for the Sun velocity with respect to the Local Standard of Rest. We will then define the Hill radius and Sphere Of Influence radius by making use of the restricted three-body theorem. We will thus have a complete model in terms of star density and distribution, kinematics, and dynamics which will lead us to quantify different mass ranges which will show the possibility of a close SNII explosion, and will highlight the perturbing effect of near low mass stars onto the Solar System Oort cloud and the action of the Sun onto alien Oort clouds. Lastly, in this thesis, we will compare our models to the latest Gaia EDR3 data which will allow us to analyze the current situation in the Solar neighborhood and will highlight the presence of stars currently perturbing the Oort cloud and five possible Solar System Oort cloud-alien Oort cloud merging.