Pushing the Frontiers of Non-equilibrium Dynamics of Collisionless and Weakly Collisional Self-gravitating Systems (2402.08766v1)

Abstract: In the standard cosmological paradigm, structure formation occurs via gravitational encounters and mergers between galaxies and dark matter halos. These collisionless self-gravitating systems therefore prevail in a state of non-equilibrium or quasi-equilibrium at best. Recent observations show that even our own Milky Way galaxy harbors non-equilibrium features. This calls for a shift of gear from the standard equilibrium galactic dynamics to the less explored non-equilibrium dynamics. This dissertation presents novel theories to describe the relaxation/equilibration of perturbed galaxies (via phase-mixing, Landau damping, etc.) in the impulsive, adiabatic and near-resonant regimes, as well as the back reaction of the host galaxy response on the perturber, resulting in its secular evolution (dynamical friction). First, we present a non-perturbative treatment of penetrating impulsive encounters between galaxies, a generalization of the standard theory which only works for distant encounters. Next, a general perturbative formalism for the phase-mixing of the response of disk galaxies to external perturbations (e.g., satellite impacts) is presented, which describes the formation and evolution of non-equilibrium features called phase-spirals akin to those discovered in our Milky Way galaxy by Gaia. Finally, we present a self-consistent perturbative theory and a non-perturbative orbit-based treatment of the near-resonant galaxy response and dynamical friction. These theories, for the first time, explain the origin of dynamical buoyancy and core-stalling, phenomena observed in $N$-body simulations of the dynamical friction of massive perturbers in cored galaxies that are unexplained in the standard Chandrasekhar and resonance theories. These processes have profound astrophysical implications, e.g., they can stall and potentially choke supermassive black hole mergers in cored galaxies.