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Astrophysical environments, such as the circumgalactic medium or galactic winds, are often multiphase with a colder phase embedded in a volume filling hot environment. In such (turbulent) systems, hydrodynamical instabilities can, on the one hand, destroy the cold gas efficiently but on the other hand radiative cooling can (re)form cold gas. In this talk, I want to discuss what sets the mass transfer between the phases, and under which conditions the cold gas can survive. I will show that the survival criterion sets a characteristic scale of cold gas but the dynamics and growth will lead to a scale-free mass distribution. I will discuss implications for
observations of the CGM, and convergence criteria for large scale (cosmological) simulations.