Speaker
Description
Observations from radio to X-ray have shown that multiphase material is present in the proximity of the center of our Galaxy and it is likely associated with strong galactic outflows. Such an environment represents therefore a unique and ideal laboratory to study in detail the physics of feedback and multiphase gas. To this purpose, we have developed self-consistent semi-analytical models of the dynamics of a multiphase wind, based on the results of state-of-the-art hydrodynamical simulations and on a recent analytical framework that describes the exchange of energy, mass and momentum between the different gas phases. Through Bayesian inference, we directly compare the outputs of such parametric models with the observations of a population of HI high-velocity clouds, recently detected through 21-cm observations close to the galactic center, up to heights of about 1.5 kpc. As I will show in my talk, we find that, assuming realistic mass and energy loading factors, SN-driven winds powered by the star formation in the central molecular zone of the Galaxy can successfully reproduce the velocities, locations and masses of the observed HI clouds, with the hot gas entraining and accelerating the cold clouds through drag force and mixing. This comparison therefore allows us to interpret for the first time these observations with a physical model and to study the feedback processes and their underlying physics with an unprecedented detail.
