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• W3103685061 abstract "We study the dynamics of phase transitions in the interstellar medium by means of three-dimensional hydrodynamic numerical simulations. We use a realistic cooling function and generic nonequilibrium initial conditions to follow the formation history of a multiphase medium in detail in the absence of gravity. We outline a number of qualitatively distinct stages of this process, including a linear isobaric evolution, transition to an isochoric regime, formation of filaments and voids (also known as thermal pancakes), the development and decay of supersonic turbulence, an approach to pressure equilibrium, and final relaxation of the multiphase medium. We find that 1%-2% of the initial thermal energy is converted into gas motions in one cooling time. The velocity field then randomizes into turbulence that decays on a dynamical timescale Ek ∝ t-α, 1 ≲ α ≲ 2. While not all initial conditions yield a stable two-phase medium, we examine such a case in detail. We find that the two phases are well mixed with the cold clouds possessing a fine-grained structure near our numerical resolution limit. The amount of gas in the intermediate unstable phase roughly tracks the rms turbulent Mach number, peaking at 25% when rms ~ 8 and decreasing to 11% when rms ~ 0.4." @default.
• W3103685061 created "2020-11-23" @default.
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• W3103685061 date "2002-04-20" @default.
• W3103685061 modified "2023-09-23" @default.
• W3103685061 title "Thermal Instability–induced Interstellar Turbulence" @default.
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• W3103685061 doi "https://doi.org/10.1086/340785" @default.
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