SIMBAD references

2003ApJ...587..278W - Astrophys. J., 587, 278-311 (2003/April-2)

Neutral atomic phases of the interstellar medium in the Galaxy.

WOLFIRE M.G., McKEE C.F., HOLLENBACH D. and TIELENS A.G.G.M.

Abstract (from CDS):

Much of the interstellar medium in disk galaxies is in the form of neutral atomic hydrogen, H I. This gas can be in thermal equilibrium at relatively low temperatures, T≲300 K (the cold neutral medium [CNM]), or at temperatures somewhat less than 104 K (the warm neutral medium [WNM]). These two phases can coexist over a narrow range of pressures, Pmin≤P≤Pmax. We determine Pminand Pmaxin the plane of the Galaxy as a function of Galactocentric radius R using recent determinations of the gas heating rate and the gas-phase abundances of interstellar gas. We provide an analytic approximation for Pminas a function of metallicity, far-ultraviolet radiation field, and the ionization rate of atomic hydrogen. Our analytic results show that the existence of Pmin, or the possibility of a two-phase equilibrium, generally requires that H+ exceed C+ in abundance at Pmin. The abundance of H+ is set by EUV/soft X-ray photoionization and by recombination with negatively charged polycyclic aromatic hydrocarbons. In order to assess whether thermal or pressure equilibrium is a realistic assumption, we define a parameter Υ≡tcool/tshock, where tcoolis the gas cooling time and tshockis the characteristic shock time or ``time between shocks in a turbulent medium.'' For Υ<1 gas has time to reach thermal balance between supernova-induced shocks. We find that this condition is satisfied in the Galactic disk, and thus the two-phase description of the interstellar H I is approximately valid even in the presence of interstellar turbulence. Observationally, the mean density n_HI_is often better determined than the local density, and we cast our results in terms of n_HI_as well. Over most of the disk of the Galaxy, the H I must be in two phases: the weight of the H I in the gravitational potential of the Galaxy is large enough to generate thermal pressures exceeding Pmin, so that turbulent pressure fluctuations can produce cold gas that is thermally stable; and the mean density of the H I is too low for the gas to be all CNM. Our models predict the presence of CNM gas to R≃16-18 kpc, somewhat farther than previous estimates. An estimate for the typical thermal pressure in the Galactic plane for 3kpc≲R≲18 kpc is Pth/k≃1.4x104exp(-R/5.5kpc) K.cm–3. At the solar circle, this gives Pth/k≃3000 K.cm–3. We show that this pressure is consistent with the C I*/C Itotratio observed by Jenkins & Tripp and the CNM temperature found by Heiles & Troland. We also examine the potential impact of turbulent heating on our results and provide parameterized expressions for the heating rate as a function of Galactic radius. Although the uncertainties are large, our models predict that including turbulent heating does not significantly change our results and that thermal pressures remain above Pminto R≃18 kpc.

Abstract Copyright:

Journal keyword(s): ISM: Clouds - ISM: General - ISM: Structure

Simbad objects: 10

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2021.07.24-04:37:15

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