Simulating galactic dust grain evolution on a moving mesh

McKinnon, R.; Vogelsberger, Mark; Torrey, Paul; Marinacci, Federico; Kannan, Rahul

doi:10.1093/mnras/sty1248

Cited by 131 publications

(147 citation statements)

References 215 publications

(424 reference statements)

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“…Other physics: Additional physical processes considered in some cosmological simulations of galaxy formation are, for example, dust physics [265][266][267][268][269][270][271][272][273] , thermal conduction 188,225,[274][275][276][277][278] , and viscosity [279][280][281][282] . Dust has typically been neglected in galaxy formation simulations since it contributes only about ∼ 1% to the mass budget of the interstellar medium.…”

Section: Radiation Hydrodynamics Equationsmentioning

confidence: 99%

Cosmological simulations of galaxy formation

et al. 2020

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Over the last decades, cosmological simulations of galaxy formation have been instrumental for advancing our understanding of structure and galaxy formation in the Universe. These simulations follow the nonlinear evolution of galaxies modeling a variety of physical processes over an enormous range of scales. A better understanding of the physics relevant for shaping galaxies, improved numerical methods, and increased computing power have led to simulations that can reproduce a large number of observed galaxy properties. Modern simulations model dark matter, dark energy, and ordinary matter in an expanding space-time starting from well-defined initial conditions. The modeling of ordinary matter is most challenging due to the large array of physical processes affecting this matter component. Cosmological simulations have also proven useful to study alternative cosmological models and their impact on the galaxy population. This review presents a concise overview of the methodology of cosmological simulations of galaxy formation and their different applications. arXiv:1909.07976v4 [astro-ph.GA] 23 Oct 2019 become important for cosmological studies since they can, for example, explore the impact of alternative cosmological models on the galaxy population. Cosmological simulations of galaxy formation therefore provide important insights into a wide range of problems in astrophysics and cosmology. The most important components of cosmological galaxy formation simulations are discussed in this review. A schematic overview of the different ingredients of cosmological simulations is presented in Figure 2. Cosmological FrameworkCosmological simulations of galaxy formation are performed within a cosmological model and start from specific initial conditions. Both of these ingredients are now believed to be known to high precision. Cosmological ModelVarious observations revealed that our Universe is geometrically flat and dominated by dark matter and dark energy accounting for about ∼ 95% of the energy density. Standard model particles make up for the remaining ∼ 5% and are collectively referred to as baryons. The leading model for structure formation assumes that dark matter is cold, with negligible random motions when decoupled from other matter, and collisionless, so-called cold dark matter, and dark energy is represented by a cosmological constant Λ, which drives the accelerated expansion of the Universe. This leads to the concordance ΛCDM model, which builds the framework for galaxy formation. Measurements of the cosmic microwave background combined with other observations such as the distance-redshift relation from Type Ia supernovae, abundances of galaxy clusters, and galaxy clustering constrain the fundamental parameters of the ΛCDM model 3 . Initial ConditionsInitial conditions for cosmological simulations specify the perturbations imposed on top of a homogeneous expanding background. The background model is generally taken to be a spatially flat Friedmann-Lemaître-Robertson-Walker space-time with a defined compositio...

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Section: Radiation Hydrodynamics Equationsmentioning

confidence: 99%

Cosmological simulations of galaxy formation

et al. 2020

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“…At the end of stellar evolution, metals and dust are then distributed in the surroundings of a star forming region by using a spline-type kernel of the SPH scheme and by weighting over 64 neighbours according to the influence region of each particle. The dust distribution simply follows the atomic metal spreading without accounting for any momentum transfer through dust grains (see McKinnon et al 2018 for a recent implementation that accounts for dynamical forces acting on dust particles). At the same time, dusty particles associated with galactic winds evolve in their hot phase through sputtering.…”

Section: Spreading Of Atomic Metals and Dust By Galactic Windsmentioning

confidence: 99%

The assembly of dusty galaxies at z ≥ 4: statistical properties

Graziani

Schneider

Ginolfi

et al. 2020

Monthly Notices of the Royal Astronomical Society

103

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The recent discovery of high redshift dusty galaxies implies a rapid dust enrichment of their interstellar medium (ISM). To interpret these observations, we run a cosmological simulation in a 30h −1 cMpc/size volume down to z ≈ 4. We use the hydrodynamical code dustyGadget, which accounts for the production of dust by stellar populations and its evolution in the ISM. We find that the cosmic dust density parameter (Ω d ) is mainly driven by stellar dust at z 10, so that mass-and metallicity-dependent yields are required to assess the dust content in the first galaxies. At z 9 the growth of grains in the ISM of evolved systems (Log(M ⋆ /M ⊙ ) > 8.5) significantly increases their dust mass, in agreement with observations in the redshift range 4 z < 8. Our simulation shows that the variety of high redshift galaxies observed with ALMA can naturally be accounted for by modeling the grain-growth timescale as a function of the physical conditions in the gas cold phase. In addition, the trends of dust-to-metal (DTM) and dust-to-gas (D) ratios are compatible with the available data. A qualitative investigation of the inhomogeneous dust distribution in a representative massive halo at z ≈ 4 shows that dust is found from the central galaxy up to the closest satellites along polluted filaments with Log(D) −2.4, but sharply declines at distances d 30 kpc along many lines of sight, where Log(D) −4.0.

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“…Consequently, the ISM shows a wide range of gas densities even within cold MCs or the diffuse ISM. Models of interstellar grain growth usually rely on an assumption that the exact gas-density field can be replaced with the mean density, which "erases" small-scale variations and other effects of dynamics (but please note the recent examples of inhomogeneous models, e.g., Zhukovska et al 2016;McKinnon et al 2018, although these studies consider variations on much large scales). If the density variations are relatively small, this approach is without a doubt very reasonable.…”

Section: Gasmentioning

confidence: 99%

Galactic dust evolution with rapid dust formation in the interstellar medium due to hypersonic turbulence

Mattsson

2019

Monthly Notices of the Royal Astronomical Society

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Turbulence can significantly accelerate the growth of dust grains by accretion of molecules. For dust dynamically coupled to the gas, the growth rate scales with the square of the Mach number, which means that the growth timescale can easily be reduced by more than an order of magnitude. The limiting timescale is therefore rather the rate of molecular cloud formation, which means that dust production in the ISM can rapidly reach the levels needed to explain the dust masses observed at high redshifts. Thus, turbulence may be the solution to the replenishment problem in models of dust evolution in high-redshift galaxies and explain the dust masses seen at z = 7 − 8. A simple analytic galactic dust-evolution model is presented, where grain growth nicely compensates for the expected higher rate of dust destruction by supernova shocks. This model is simpler, relies on fewer assumptions and seems to yields a better fit to data derived from observations, compared to previous models of the same type.

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Simulating galactic dust grain evolution on a moving mesh

Cited by 131 publications

References 215 publications

Cosmological simulations of galaxy formation

Cosmological simulations of galaxy formation

The assembly of dusty galaxies at z ≥ 4: statistical properties

Galactic dust evolution with rapid dust formation in the interstellar medium due to hypersonic turbulence

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