scholarly journals Scaling laws of passive-scalar diffusion in the interstellar medium

2017 ◽  
Vol 467 (2) ◽  
pp. 2421-2429 ◽  
Author(s):  
Matthew J. Colbrook ◽  
Xiangcheng Ma ◽  
Philip F. Hopkins ◽  
Jonathan Squire
Keyword(s):  
Interstellar Medium ◽  
Scaling Laws ◽  
Passive Scalar ◽  
Scalar Diffusion

A multi-relaxation lattice kinetic method for passive scalar diffusion

2005 ◽  
Vol 206 (2) ◽  
pp. 453-462 ◽  
Author(s):  
Igor Rasin ◽  
Sauro Succi ◽  
Wolfram Miller
Keyword(s):  
Kinetic Method ◽  
Passive Scalar ◽  
Scalar Diffusion

scholarly journals JINGLE – IV. Dust, H i gas, and metal scaling laws in the local Universe

2020 ◽  
Vol 496 (3) ◽  
pp. 3668-3687 ◽  
Author(s):  
I De Looze ◽  
I Lamperti ◽  
A Saintonge ◽  
M Relaño ◽  
M W L Smith ◽  
...  
Keyword(s):  
Interstellar Medium ◽  
Grain Growth ◽  
Scaling Laws ◽  
Formation Rate ◽  
Growth Time ◽  
Dust Production ◽  
Reverse Shock ◽  
Local Scaling ◽  
Nearby Galaxies ◽  
Stellar Sources

ABSTRACT Scaling laws of dust, H i gas, and metal mass with stellar mass, specific star formation rate, and metallicity are crucial to our understanding of the build-up of galaxies through their enrichment with metals and dust. In this work, we analyse how the dust and metal content varies with specific gas mass (MH i/M⋆) across a diverse sample of 423 nearby galaxies. The observed trends are interpreted with a set of Dust and Element evolUtion modelS (DEUS) – including stellar dust production, grain growth, and dust destruction – within a Bayesian framework to enable a rigorous search of the multidimensional parameter space. We find that these scaling laws for galaxies with −1.0 ≲ log MH i/M⋆ ≲ 0 can be reproduced using closed-box models with high fractions (37–89 ${{\ \rm per\ cent}}$) of supernova dust surviving a reverse shock, relatively low grain growth efficiencies (ϵ = 30–40), and long dust lifetimes (1–2 Gyr). The models have present-day dust masses with similar contributions from stellar sources (50–80 ${{\ \rm per\ cent}}$) and grain growth (20–50 ${{\ \rm per\ cent}}$). Over the entire lifetime of these galaxies, the contribution from stardust (>90 ${{\ \rm per\ cent}}$) outweighs the fraction of dust grown in the interstellar medium (<10 ${{\ \rm per\ cent}}$). Our results provide an alternative for the chemical evolution models that require extremely low supernova dust production efficiencies and short grain growth time-scales to reproduce local scaling laws, and could help solving the conundrum on whether or not grains can grow efficiently in the interstellar medium.

Passive-scalar diffusion in a fluid membrane

2002 ◽  
Vol 116 (18) ◽  
pp. 7787-7794 ◽  
Author(s):  
Youhei Fujitani
Keyword(s):  
Passive Scalar ◽  
Fluid Membrane ◽  
Scalar Diffusion

scholarly journals THE PROPERTIES OF THE STAR-FORMING INTERSTELLAR MEDIUM ATz= 0.8–2.2 FROM HiZELS: STAR FORMATION AND CLUMP SCALING LAWS IN GAS-RICH, TURBULENT DISKS

2012 ◽  
Vol 760 (2) ◽  
pp. 130 ◽  
Author(s):  
A. M. Swinbank ◽  
Ian Smail ◽  
D. Sobral ◽  
T. Theuns ◽  
P. N. Best ◽  
...  
Keyword(s):  
Star Formation ◽  
Interstellar Medium ◽  
Scaling Laws ◽  
Star Forming

scholarly journals Passive Scalar Diffusion as a Damped Wave

2005 ◽  
pp. 3-6
Author(s):  
Axel Brandenburg ◽  
Petri J. Käpylä ◽  
Amjed Mohammed
Keyword(s):  
Passive Scalar ◽  
Scalar Diffusion

scholarly journals Modelling and Experimental Validation of a Passive Scalar Diffusion

2012 ◽  
Vol 7 (5) ◽  
pp. 363-371
Author(s):  
D. Tcheukam- Toko ◽  
C.A. Koueni-Tok ◽  
R. Mouangue ◽  
P. Paranthoen
Keyword(s):  
Experimental Validation ◽  
Passive Scalar ◽  
Scalar Diffusion

scholarly journals Turbulence in nearly incompressible fluids: density spectrum, flows, correlations and implication to the interstellar medium

2005 ◽  
Vol 12 (1) ◽  
pp. 139-148 ◽  
Author(s):  
S. Dastgeer ◽  
G. P. Zank
Keyword(s):  
Interstellar Medium ◽  
Pressure Fluctuations ◽  
Thermal Fluctuation ◽  
Passive Scalar ◽  
Density Fluctuations ◽  
Density Spectrum ◽  
Electron Density Fluctuations ◽  
Nonlinear Fluid ◽  
Solar Wind Electron

Abstract. Interstellar scintillation and angular radio wave broadening measurements show that interstellar and solar wind (electron) density fluctuations exhibit a Kolmogorov-like k-5/3 power spectrum extending over many decades in wavenumber space. The ubiquity of the Kolmogorov-like interstellar medium (ISM) density spectrum led to an explanation based on coupling incompressible magnetohydrodynamic (MHD) fluctuations to density fluctuations through a "pseudosound" relation within the context of "nearly incompressible" (NI) hydrodynamics (HD) and MHD models. The NI theory provides a fundamentally different explanation for the observed ISM density spectrum in that the density fluctuations can be a consequence of passive scalar convection due to background incompressible fluctuations. The theory further predicts generation of long-scale structures and various correlations between the density, temperature and the (magneto) acoustic as well as convective pressure fluctuations in the compressible ISM fluids in different thermal regimes that are determined purely by the thermal fluctuation level. In this paper, we present the results of our two dimensional nonlinear fluid simulations, exploring various nonlinear aspects that lead to inertial range ISM turbulence within the context of a NI hydrodymanics model. In qualitative agreement with the NI predictions and the in-situ observations, we find that i) the density fluctuations exhibit a Kolmogorov-like spectrum via a passive convection in the field of the background incompressible fluctuations, ii) the compressible ISM fluctuations form long scale flows and structures, and iii) the density and the temperature fluctuations are anti-correlated.

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