Numerical Models of the Multiphase Interstellar Matter with Stellar Energy Feedback on a Galactic Scale

By K. Wada, C. Norman. 2001

209 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

Turbulent Structure of a Stratified Supernova-driven Interstellar Medium (2005, methodology): “Several authors have arguedthat only a fixed (constant) fraction of massfM above some density threshold will collapse to form stars (Elmegreen 2002; Krumholz & McKee 2005), based on the universality of density PDFs in turbulent media (Wada & Norman 2001).”
THE DISRUPTION OF GIANT MOLECULAR CLOUDS BY RADIATION PRESSURE & THE EFFICIENCY OF STAR FORMATION IN GALAXIES (2009, background): “…massive stars, depositi n of momentum by expanding bubbles of photoionized HII region gas, deposition of momentum by the shocked winds from massive stars, and jets from protostars (e.g., McKee & Ostriker 1977; Silk 1997; Wada & Norman 2001; Matzner 2002; Li & Nakamura 2006; Cunningham et al. 2008).”
Radiative feedback and the low efficiency of galaxy formation in low-mass haloes at high redshift (2013, background): “Overall, the distributions are close to log-normal (Wada & Norman 2001), with a peak around0.”
Rapid Formation of Molecular Clouds and Stars in the Solar Neighborhood (2001, background): “Much, if not most, of the stellar energy input into the interstellar medium arises from super- novae (Spitzer 1978; Wada & Norman 2001).”
ENVIRONMENTAL DEPENDENCE OF THE KENNICUTT–SCHMIDT RELATION IN GALAXIES (2010, background): “The minimal model is often (justifiably) used in studies of local ISM (c.f. Krumholz & McKee 2005; Pelupessy et al. 2006; Krumholz & Tan 2007; Glover & Mac Low 2007a,b), but is also occasionally applied to high-redshift or low-metallicity systems (Krumholz et al. 2009a; Pelupessy & Papadopoulos 2009”
Circumnuclear Dust in Nearby Active and Inactive Galaxies. II. Bars, Nuclear Spirals, and the Fueling of Active Galactic Nuclei (2002, background): “The possibility of shock-driven inflow, as traced by nuclear spiral structure, has been the subject of a number of recent theoretical studies (Fukuda et al. 1998; Montenegro, Yuan, & Elmegreen 1999; Wada & Norman 2001; Maciejewski et al. 2002; Wada, Meurer, & Norman 2002).”
Towards simulating star formation in the interstellar medium (2004, methodology): “In three-dimensional simulations of a high-redshift galaxy performed in a cosmological context, Kravtsov (2003) ﬁnds a density distribution similar to Wada & Norman (2001).”
On the Origin of the Global Schmidt Law of Star Formation (2003, methodology): “In particular, it is very similar to the density PDF in the 2D disk simulations of Wada & Norman (2001).”
Interstellar Turbulence I: Observations and Processes (2004, background): “Simulation codes are finally becoming sophisticated enough to model at least the central regions of differentially rotating galaxies, with simulations of 2 kpc x 2 kpc up to 40962 (Wada & Norman 2001, Wada et al. 2002).”
A sub-parsec resolution simulation of the Milky Way: global structure of the interstellar medium and properties of molecular clouds (2013, background): “Log-normals generally provide good fits to PDFs of simulated isothermal, supersonically turbulent gas (among many others, see Vazquez-Semadeni 1994; Nordlund & Padoan 1999; Wada & Norman 2001).”
Collapse and Fragmentation in Finite Sheets (2004, background): “The resulting clouds are then formed as wall sections of “bubbles” (e.g. Vazquez-Semadeni, Passot, & Pouquet 1995; Passot, Vasquez-Semadeni, & Pouquet 1995; de Avillez & Mac Low 2001; Wada & Norman 2001; HBB01, and references therein).”
Three-Dimensional Simulations of a Starburst-driven Galactic Wind (2008, background): “Moreover, the concept of supersonic turbulence is not new in the context of starburst galaxies and is a key feature of the simulations of the ISM in such galaxies (e.g., Wada & Norman 2001, 2007).”
THE IMPACT OF INTERACTIONS, BARS, BULGES, AND ACTIVE GALACTIC NUCLEI ON STAR FORMATION EFFICIENCY IN LOCAL MASSIVE GALAXIES (2012, result): “…et al. (2011) find the probability distribution function (PDF) of the local gas density in mergers to be broader and shifted to higher densities (or perhaps to have a different functional form), compared to the mostly log-normal PDFs found in normal star-forming galaxies (Wada & Norman 2001).”
The Supernova Rate-Velocity Dispersion Relation in the Interstellar Medium (2005, unknown): “Wada & Norman (1999, 2001) 1 Max-Planck-Institut f ür Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany; dib@mpia.de, bell@mpia.de.”
THE ROLE OF STELLAR FEEDBACK IN THE FORMATION OF GALAXIES (2007, background): “However, these turbulent driven shocks can only heat the gas up to 106 K (Wada & Norman 2001).”
The Second Survey of the Molecular Clouds in the Large Magellanic Cloud by NANTEN. I. Catalog of Molecular Clouds (2008, background): “According to Wada & Norman (2001), the absence of a massive GMC of ∼ 3 × 106 M⊙ is due to the well-mixed, turbulent interstellar medium that tends to form smaller GMCs.”
The properties of satellite galaxies in simulations of galaxy formation (2009, background): “On the other hand, Wada & Norman (2001, 2007) suggested that the multi-phase ISM is supported by turbulent motions induced by the self-gravity of the gas and galactic rotation.”