THE THREE-PHASE INTERSTELLAR MEDIUM REVISITED

By D. Cox. 2005

309 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c448dacab85c352a16cbecfe0ffe8a3ec43f2942

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Citations in the corpus

GLOBAL COSMIC-RAY-RELATED LUMINOSITY AND ENERGY BUDGET OF THE MILKY WAY (2010, background): “…fill up the entire volume of galaxies, providing an important source of heating and ionisation of the interstellar medium (ISM), and may play a significant role in the regulation of star formation and evolution of galaxies (Ferrière 2001; Cox 2005; Socrates et al. 2008; Sironi & Socrates 2010).”
A far-infrared survey of bow shocks and detached shells around AGB stars and red supergiants (Corrigendum) (2011, background): “The different phases of the ISM have different average densities, scale-heights and filling factors (see e.g. Savage 1995; Boulanger 2001; Ferrière 2001; Wooden et al. 2004; Cox 2005).”
The Milky Way’s Kiloparsec-Scale Wind: A Hybrid Cosmic-Ray and Thermally Driven Outflow (2007, background): “We estimate that at the Sun’s position in the Galaxy, Pg,⊙/kB ∼ 7000 cm−3 K (Cox 2005, in his §4.2).”
Planck intermediate results. XIX. An overview of the polarized thermal emission from Galactic dust (2014, unknown): “With a pressure larger than the thermal pressure of all phases and comparable to that of the cosmic rays (Cox 2005), the Galactic magnetic field (GMF) plays a crucial role in the ecosystem of our Galaxy.”
Terahertz Spectroscopy for Astronomy: From Comets to Cosmology (2011, background): “The interstellar medium in the Galaxy is a patchy, clumpy medium that encompasses extremes of temperature and a wide range of densities [28].”
Global properties of the H I distribution in the outer Milky Way - Planar and extra-planar gas (2008, methodology): “This model is currently favored for ISM research (Cox 2005, Sect.”
Turbulent molecular clouds (2012, background): “Because it sits in the gravitational potential of the Galaxy and extends up to ∼ 300 pc above the plane, the diffuse ISM has to be supported by a pressure that is about 10 times its thermal pressure, Ptot = 3 × 10−12 dynes cm−2, or Ptot/k ∼ 2 × 104 cm−3 K (Cox 2005).”
Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, background): “Massive star feedback may also terminate star formation locally, blowing giant bubbles (Cox 2005) and leaking hot processed gas into the Galactic Halo (Putman et al. 2012).”
THE ROLE OF STELLAR FEEDBACK IN THE FORMATION OF GALAXIES (2007, methodology): “The galactic ISM has a very wide range of densities and temperatures (for review see Cox 2005 and Ferrière 2001).”
Magnetism in the spiral galaxy NGC 6946: magnetic arms, depolarization rings, dynamo modes, and helical fields (2007, background): “The energy densities of all components in NGC 6946 are about one order of magnitude larger than in the Milky Way (Cox 2005).”
The Sydney-AAO Multi-object Integral field spectrograph (2011, background): “The gas may arise from some kind of disc-wide interaction between the disc and the hot halo, presumably driven by processes related to star formation in the disc (Cox 2005).”
The Vertical Structure of Warm Ionised Gas in the Milky Way (2008, background): “Other estimates for the pressure of the WIM and of other ISM phases show a wide variation depending on local conditions, but certainly the above value falls comfortably within the typically observed range (see Cox 2005).”
STAR FORMATION IN DISK GALAXIES. I. FORMATION AND EVOLUTION OF GIANT MOLECULAR CLOUDS VIA GRAVITATIONAL INSTABILITY AND CLOUD COLLISIONS (2008, background): “While the clouds do largely reside in the plane of the disk (which is in essence a two-dimensional system), cloud collisions and feedback can eject gas from the surface, a process that controls the pressure of the ISM from which the clouds are forming (McKee & Ostriker 1977; Cox 2005).”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “In the Milky Way, about half the volume is filled by a hot ionized medium (HIM) with n < 0.01 cm−3 and TK > 10 5 K, and half is filled by some combination of warm ionized medium (WIM) and warm neutral medium (WNM), with n ∼ 0.1 − 1 cm−3 and TK of several thousand K (Cox 2005).”
MOMENTUM INJECTION BY SUPERNOVAE IN THE INTERSTELLAR MEDIUM (2014, background): “The addition of SN-driven shocks to the ISM makes its inhomogeneity even more extreme, producing a third phase of extremely tenuous gas (McKee & Ostriker 1977; Cox 2005).”
Diffuse Atomic and Molecular Clouds (2006, background): “These phases are thought to be in approximate pressure equilibrium with one another (see Savage & Sembach 1996 or Cox 2005 for a general description of the physical conditions and phases in the galactic ISM).”
The warm ionized medium in spiral galaxies (2009, background): “Cox and Helenius (2003) and Lockman (2004), for example, have suggested that portions of the ionized medium may condense into neutral clouds.”
Galactic winds driven by cosmic ray streaming (2012, background): “This is expected given the near equipartition of energy in the Milky Way disc between magnetic fields, CRs and the thermal pressure (Zweibel & Heiles 1997; Beck 2001; Cox 2005).”