Interstellar Turbulence II: Implications and Effects

By J. Scalo, B. S. I. O. Astronomy, U. Texas, I. T. R. Center. 2004

270 citations recorded by the source corpus.

▪ Abstract Interstellar turbulence has implications for the dispersal and mixing of the elements, cloud chemistry, cosmic ray scattering, and radio wave propagation through the ionized medium. This review discusses the observations and theory of these effects. Metallicity fluctuations are summarized, and the theory of turbulent transport of passive tracers is reviewed. Modeling methods, turbulent concentration of dust grains, and the turbulent washout of radial abundance gradients are discussed. Interstellar chemistry is affected by turbulent transport of various species between environments with different physical properties and by turbulent heating in shocks, vortical dissipation regions, and local regions of enhanced ambipolar diffusion. Cosmic rays are scattered and accelerated in turbulent magnetic waves and shocks, and they generate turbulence on the scale of their gyroradii. Radio wave scintillation is an important diagnostic for small-scale turbulence in the ionized medium, giving information abou...

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/58c99f76b576b719526ebd9e7d4cd33cb25129b6

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Citations in the corpus

Comparing the statistics of interstellar turbulence in simulations and observations - Solenoidal versus compressive turbulence forcing (2009, background): “The role of supersonic turbulence in star formation is summarised in the review articles by Mac Low & Klessen (2004), Elmegreen & Scalo (2004), Scalo & Elmegreen (2004) and McKee & Ostriker (2007).”
The Stellar Mass Spectrum from Non-Isothermal Gravoturbulent Fragmentation (2004, background): “The observed turbulent velocity field in molecular clouds will decay in a crossing time if not continuously replenished (Mac Low & Klessen 2004; Scalo & Elmegreen 2004; Elmegreen & Scalo 2004).”
Turbulent molecular clouds (2012, background): “Other comprehensive references on closely related topics can be found in Mac Low & Klessen (2004), Elmegreen & Scalo (2004), Scalo & Elmegreen (2004), McKee & Ostriker (2007) and Kennicutt & Evans (2012).”
Resolving the Formation of Protogalaxies. III. Feedback from the First Stars (2007, unknown): “Fortunately the dispersion of heavy elements from SNe into the Galactic ISM is a rich field of study (for a review, see Scalo & Elmegreen 2004).”
THE FRACTAL DENSITY STRUCTURE IN SUPERSONIC ISOTHERMAL TURBULENCE: SOLENOIDAL VERSUS COMPRESSIVE ENERGY INJECTION (2007, background): “These motions are associated with compressible turbulence (e.g., Elmegreen & Scalo 2004; Scalo & Elmegreen 2004; Mac Low & Klessen 2004) in the interstellar medium (Ferrière 2001) and exhibit a single turbulent cascade or spatially separated coexisting inertial ranges (Passot et al. 1988) similar…”
Evolution of interstellar dust and stardust in the solar neighbourhood (2007, background): “The small scatter of abundances between stars in open stellar clusters indicate, however, that the intrinsic scatter seems to be very small (see Scalo & Elmegreen 2004, and references therein); we arbitrarily assume a contribution of 0.1 dex to the total scatter.”
The Stellar IMF, Core Mass Function, & The Last-Crossing Distribution (2012, background): “It is increasingly clear that the density structure of the ISM is dominated by supersonic turbulence over a wide range of scales (e.g. Scalo & Elmegreen 2004; Elmegreen & Scalo 2004; Mac Low & Klessen 2004; McKee & Ostriker 2007), and a fairly generic consequence of this is that the density…”
Theory of Star Formation (2007, background): “A much more extensive literature survey and discussion of interstellar turbulence, including both diffuse-ISM and dense-ISM regimes, is presented by Elmegreen & Scalo (2004) and Scalo & Elmegreen (2004).”
IONIZING PHOTON ESCAPE FRACTIONS FROM HIGH-REDSHIFT DWARF GALAXIES (2008, background): “Turbulent energy— Initial turbulent energy should be unimportant in the more massive halos as radiative and SN feedback continuously alters the ISM and further stirs turbulence (e.g. Scalo & Elmegreen 2004), perhaps overpowering any pre-existing turbulence.”
Present-day cosmic abundances - A comprehensive study of nearby early B-type stars and implications for stellar and Galactic evolution and interstellar dust models (2012, background): “Theoretical investigations of metal abundance fluctuations in the ISM have until recently been based on order of magnitude arguments involving characteristic spatial scales and timescales for various turbulent mixing processes, see e.g. Roy & Kunth (1995), and Scalo & Elmegreen (2004) for a review.”
Accretion-driven turbulence as universal process: galaxies, molecular clouds, and protostellar disks (2009, background): “Several possibilities have been discussed (Elmegreen & Scalo 2004; Mac Low & Klessen 2004; Scalo & Elmegreen 2004).”
MODELING COLLAPSE AND ACCRETION IN TURBULENT GAS CLOUDS: IMPLEMENTATION AND COMPARISON OF SINK PARTICLES IN AMR AND SPH (2010, background): “Supersonic turbulence, in particular, plays an important role in shaping the cloud structure, and in controlling star formation, because it creates the seeds for local gravitational collapse (Elmegreen & Scalo 2004; Scalo & Elmegreen 2004; Mac Low & Klessen 2004; McKee & Ostriker 2007).”
FORMATION OF MASSIVE MOLECULAR CLOUD CORES BY CLOUD–CLOUD COLLISION (2013, background): “The power spectrum of the density fluctuations is set as an isotropic power law: (logρ)2k k 2 ∝ k−2 (Larson 1981; Heyer & Brunt 2004), which can be expected by supersonic turbulence that follows Larson’s law (Beresnyak et al. 2005, see also, Elmegreen & Scalo 2004; Scalo & Elmegreen 2004).”
Modelling CO formation in the turbulent interstellar medium (2009, background): “…picture has begun to give way to a new picture of clouds as inherently dynamical entities, whose formation and evolution are dominated by the effects of turbulence (Ballesteros-Paredes et al. 1999; Klessen, Heitsch & Mac Low 2000; Klessen 2001; Elmegreen & Scalo 2004; Scalo & Elmegreen 2004).”
Molecular Clouds in the Milky Way (2015, background): “…in relation to star formation (McKee & Ostriker 2007, Hennebelle & Falgarone 2012, Kennicutt & Evans 2012, Krumholz 2014); interstellar turbulence (Scalo & Elmegreen 2004, Elmegreen & Scalo 2004); cold, dark clouds (Bergin & Tafalla 2007); nearby galaxies (Fukui & Kawamura 2010); magnetic fields…”
Recent progress in astrophysical plasma turbulence from solar wind observations (2016, background): “…galactic magnetic field amplification (Kulsrud & Zweibel 2008), limit thermal conduction in galaxy clusters (Schekochihin et al. 2008), determine the dispersal and mixing of elements in the interstellar medium (Scalo & Elmegreen 2004), and play a key role in star formation (McKee & Ostriker 2007).”
Science with ASKAP (2008, background): “There is little doubt that interstellar turbulence plays a significant role in the structure, kinematics and global evolution of the ISM (see review papers by [89] and [235]).”