2001/06/27 by Mordecai-Mark Mac Low, Mordecai‐Mark Mac Low, Dinshaw Balsara +8 · 3 citations
Physics and Astronomy · #Astro and Planetary Science #Astrophysics (astro-ph) #Astrophysics and Star Formation Studies #FOS: Physical sciences #Gamma-ray bursts and supernovae #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0106509
Submitted to ApJ 26 June 2001. 36 pages, 13 reduced resolution color figures, contained on pages 24-36. First 23 pages can be printed on regular printer
arxiv created 2001/06/27 · openalex publication_date 2001/06/27 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
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.