Is Thermal Instability Significant in Turbulent Galactic Gas?

Abstract

We investigate numerically the role of thermal instability (TI) as a generator of density structures in the interstellar medium (ISM), both by itself and in the context of a globally turbulent medium. We consider three sets of numerical simulations: (1) —ows in the presence of the instability only; (2) —ows in the presence of the instability and various types of turbulent energy injection (forcing), and (3) models of the ISM including the magnetic —eld, the Coriolis force, self-gravity and stellar energy injection. Simula- tions in the —rst group show that the condensation process that forms a dense phase (ii clouds ˇˇ) is highly dynamical and that the boundaries of the clouds are accretion shocks, rather than static density discon- tinuities. The density histograms (probability density functions (PDFs)) of these runs exhibit either bimodal shapes or a single peak at low densities plus a slope change at high densities. Final static situ- ations may be established, but the equilibrium is very fragile: small density —uctuations in the warm phase require large variations in that of the cold phase, probably inducing shocks in the clouds. Com- bined with the likely disruption of the clouds by Kelvin-Helmholtz instability, this result suggests that such con—gurations are highly unlikely. Simulations in the second group show that large-scale turbulent forcing is incapable of erasing the signature of TI in the density PDFs, but small-scale, stellar-like forcing causes the PDFs to transit from bimodal to a single-slope power law, erasing the signature of the instability. However, these simulations do not reach stationary regimes, with TI driving an ever- increasing star formation rate. Simulations in the third group show no signi—cant diUerence between the PDFs of stable and unstable cases and reach stationary regimes, suggesting that the combination of the stellar forcing and the extra eUective pressure provided by the magnetic —eld and the Coriolis force over- whelm TI as a density-structure generator in the ISM, with TI becoming a second-order eUect. We emphasize that a multimodal temperature PDF is not necessarily an indication of a multiphase medium, which must contain clearly distinct thermal equilibrium phases, and that this ii multiphase ˇˇ terminology is often inappropriately used. Subject headings: instabilitiesISM: structureturbulence