• DOI:10.1086/430122
• Corpus ID: 14791607

The Distribution of Pressures in a Supernova-Driven Interstellar Medium

@article{Low2001TheDO,
  title={The Distribution of Pressures in a Supernova-Driven Interstellar Medium},
  author={Mordecai Mac Low and Dinshaw S. Balsara and Miguel A. de Avillez and Jongsoo Kim American Museum of Natural History and National Center for Supercomputing Applications and Notre Dame University and Korea Astronomy Observatory},
  journal={arXiv: Astrophysics},
  year={2001}
}

• M. M. Low, D. Balsara, +4 authors K. A. Observatory
• Published 27 June 2001
• Physics
• arXiv: Astrophysics

Observations have suggested substantial departures from pressure equilibrium in the interstellar medium (ISM) in the plane of the Galaxy, even on scales under 50 pc. Nevertheless, multi-phase models of the ISM assume at least locally isobaric gas. The pressure then determines the density reached by gas cooling to stable thermal equilibrium. We use two different sets of numerical models of the ISM to examine the consequences of supernova driving for interstellar pressures. The first set of models is hydrodynamical, and uses adaptive mesh refinement to allow computation of a 1 x 1 x 20 kpc section of a stratified galactic disk. The second set of models is magnetohydrodynamical, using an independent code framework, and examines a 200 pc cubed periodic domain threaded by magnetic fields. Both of these models show broad pressure distributions with roughly log-normal functional forms produced by both shocks and rarefaction waves, rather than the power-law distributions predicted by previous work, with rather sharp thermal pressure gradients. The width of the distribution of the logs of pressure in gas with log T < 3.9 is proportional to the rms Mach number in that gas, while the distribution in hotter gas is broader, but not so broad as would be predicted by the Mach numbers in that gas. Individual parcels of gas reach widely varying points on the thermal equilibrium curve: no unique set of phases is found, but rather a dynamically-determined continuum of densities and temperatures. Furthermore, a substantial fraction of the gas remains entirely out of thermal equilibrium. Our results appear consistent with observations of interstellar pressures, and suggest that the pressures observed in molecular clouds may be due to ram pressure rather than gravitational confinement.