Neutral Atomic Phases of the Interstellar Medium in the Galaxy

By M. Wolfire, C. McKee, D. Hollenbach, A. Tielens. 2003

782 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/df2e1e3d883146fa95dc60204e949213dca295fe

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

STAR FORMATION IN DISK GALAXIES. I. FORMATION AND EVOLUTION OF GIANT MOLECULAR CLOUDS VIA GRAVITATIONAL INSTABILITY AND CLOUD COLLISIONS (2008, background): “…most of the Galactic molecular gas is organized in GMCs and that GMCs have approximately equal mass atomic envelopes (Blitz 1990), the results of Wolfire et al. (2003) for the radial distribution of Galactic molecular and atomic gas indicate that a large fraction, ∼ 1/3, of the total gas mass…”
PHYSICAL PROPERTIES AND GALACTIC DISTRIBUTION OF MOLECULAR CLOUDS IDENTIFIED IN THE GALACTIC RING SURVEY (2010, background): “…i) electrons ejected from dust grains illuminated by the Interstellar Radiation Field (ISRF) due to the photoeletric effect (Bakes & Tielens 1994; Wolfire et al. 2003), ii) H2 photo-dissociation (Black & Dalgarno 1977), iii) collisions between Galactic Cosmic Rays (GCRs) and molecules (Goldsmith…”
The VLT-UVES survey for molecular hydrogen in high-redshift damped Lyman α systems: physical conditions in the neutral gas (2005, result): “…pressure range in DLA components is higher than that typically measured in the Galactic ISM (see Jenkins & Tripp 2001) and consistent with what is expected in the CNM with lower metallicity (Z ∼ 0.1 Z ) and dust depletion (see Wolfire et al. 1995, 2003; Wolfe et al. 2003a,b; Srianand et al. 2005).”
A General Theory of Turbulence-regulated Star Formation, from Spirals to Ultraluminous Infrared Galaxies (2005, methodology): “…al. 2003) hH i 65 pc; rk < 8:5; 65 exp rk 8:5 6:7 pc; rk 8:5; 8< : ð66Þ and hmol 33 pc; rk < 8:5; 33 exp rk 8:5 6:7 pc; rk 8:5: 8< : ð67Þ Note that we have converted the half-density heights given by Wolfire et al. (2003) to scale heights by assuming an isothermal density profile / sech2 ½z/(2hg) .”
EXTENDING THE NEARBY GALAXY HERITAGE WITH WISE: FIRST RESULTS FROM THE WISE ENHANCED RESOLUTION GALAXY ATLAS (2012, background): “The O and B stars emit strong ultra-violet (UV) radiation that ionizes and heats the ISM, providing the energy needed to warm dust, excite and break apart molecules thereby creating HII and photo-dissociation regions (e.g. Tielens & Hollenbach 1985; Wolfire et al. 2003).”
Molecular Hydrogen and Global Star Formation Relations in Galaxies (2007, background): “Such flaring, for example, is observed for the Milky Way atR & 10 kpc (e.g., Wolfire et al. 2003, and references therein).”
CO-dark gas and molecular filaments in Milky Way-type galaxies (2014, background): “On large scales, however, this should be a reasonable approximation provided that we consider a region within a few kpc of the Solar Galactocentric radius (Wolfire et al. 2003).”
On the fraction of star formation occurring in bound stellar clusters (2012, methodology): “The input variables for the different galaxies are as follows: (i) For the Milky Way, we use the Wolfire et al. (2003) model for the ISM, including a factor of 1.4 to account for the presence of helium, and adopt σ g = 7 km s−1 (Heiles & Troland 2003) to calculate Q.”
The big problems in star formation: The star formation rate, stellar clustering, and the initial mass function (2014, neutral): “10−4 (Wolfire et al. 2003).”
PHYSICAL PROPERTIES OF MOLECULAR CLOUDS FOR THE ENTIRE MILKY WAY DISK (2016, methodology): “We note that the value in the solar neighborhood (σ0 ≈ 0.8 km s−1) is similar to the one estimated in the more diffuse H i component (Wolfire et al. 2003; Saury et al. 2014).”
Cloud-scale Molecular Gas Properties in 15 Nearby Galaxies (2018, background): “Moreover, the ambient pressure is expected to vary as a function of location in the galaxy in response to the distribution of gas and the potential of the galaxy (e.g., Elmegreen 1989; Wolfire et al. 2003; Ostriker et al. 2010; Herrera-Camus et al. 2017; Meidt et al. 2018).”
THREE-DIMENSIONAL HYDRODYNAMIC SIMULATIONS OF MULTIPHASE GALACTIC DISKS WITH STAR FORMATION FEEDBACK. I. REGULATION OF STAR FORMATION RATES (2013, methodology): “In the analytic model for thermal/dynamical equilibrium (OML10; OS11), ηth = 1.2frad, where frad = [0.25 + 0.75Z′d (Σ/10 M pc−2)0.4]−1 using the heating/cooling model of Wolfire et al. (2003), and ηturb = 3.6fp for p∗/m∗ = 3000 km s−1.”
THE STAR FORMATION EFFICIENCY IN NEARBY GALAXIES: MEASURING WHERE GAS FORMS STARS EFFECTIVELY (2008, positive): “Therefore, instead of large-scale gravitational instability or cloud destruction by shear, the ability to form a cold neutral medium (McKee & Ostriker 1977; Wolfire et al. 2003) may regulate GMC formation.”
Cosmic-Ray Propagation: Nonlinear Diffusion Parallel and Perpendicular to Mean Magnetic Field (2007, background): “However, we accept that different parts of interstellar medium can exhibit variations of these parameters (see Wolfire et al. 2003 and ref. therein).”
[Si II], [Fe II], [C II], and H2 Emission from Massive Star-forming Regions (2006, methodology): “PDRs include the neutral dense gas near sources of intense FUV illumination and the neutral diffuse ISM (e.g., Tielens & Hollenbach 1985; Parravano et al. 2003; Wolfire et al. 2003).”
Terahertz Spectroscopy for Astronomy: From Comets to Cosmology (2011, background): “1) Efforts to study the ecology of the Galaxy will need to map on the order of 100 square degrees, necessitating the development of heterodyne arrays at terahertz frequencies.”
FORMING REALISTIC LATE-TYPE SPIRALS IN A ΛCDM UNIVERSE: THE ERIS SIMULATION (2011, methodology): “Eris’ H I mass is MHI = 1.9 × 109 M , comparable to the H I mass estimated for the Milky Way disk by Nakanishi & Sofue (2003), but smaller than the value of ∼ 5×109 M given by Wolfire et al. (2003).”
Diagnostics of irradiated gas in galaxy nuclei. I. A far-ultraviolet and X-ray dominated region code (2005, neutral): “5 of Wolfire et al. (2003) in the PDR models.”