On the treatment of entropy mixing in numerical cosmology

By James Wadsley, G. Veeravalli, Hugh M. P. Couchman. 2008

204 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Computational Mechanics

View Paper: https://www.semanticscholar.org/paper/5625f7098acdaf4c10cfbd5b356b76528d3e2e36

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Citations in the corpus

Smoothed particle hydrodynamics and magnetohydrodynamics (2010, methodology): “vity does not have to be the same as that used for the viscosity. In particular, Price (2008) proposed using vu sig = p jP a P bj=ˆ ab to equalise the pressure across contact discontinuities, whilst Wadsley et al. (2008) proposed a conductivity term equivalent to using vu sig = jv ab^r abj(we adopt ”
NIHAO - XI. Formation of ultra-diffuse galaxies by outflows (2016, unknown): “The code includes a subgrid model for turbulent mixing of metals and energy (Wadsley et al. 2008), ultraviolet heating, ionization and metal cooling (Shen et al. 2010).”
The dependence of dark matter profiles on the stellar-to-halo mass ratio: a prediction for cusps versus cores (2013, methodology): “In yellow, we include simulations withǫesf = 0.175, in which diffusion of thermal energy from gas particles (Stinson et al. 2012; Wadsley et al. 2008)is allowed to occur during the adiabatic expansion phase.”
RESIDUAL GAS MOTIONS IN THE INTRACLUSTER MEDIUM AND BIAS IN HYDROSTATIC MEASUREMENTS OF MASS PROFILES OF CLUSTERS (2009, background): “…particular, it can also be responsible for dispersing metals from the ICM core, where the abundance profile is broader than the central galaxy brightness profile (Rebusco et al. 2005) and more generally in mixing gas of different metallicity and entropy (Wadsley et al. 2008; Mitchell et al. 2008).”
The transition from population III to population II-I star formation (2010, background): “…have been don (Spitzer 1962; Cowie & McKee 1977; Brookshaw 1985; Sarazin 1988; Monaghan 1992; Cleary & Monaghan 1999; Klessen & Lin 2003; Jubelgas et al. 2004; Monaghan et al. 2005; Wadsley et al. 2008; Greif et al. 2009), but much more realistic and detailed analyses are still strongly needed.”
E pur si muove: Galilean-invariant cosmological hydrodynamical simulations on a moving mesh (2009, background): “This provides for an implicit source of entropy, with sometimes unclear consequences, a situation that prompted Wadsley et al. (2008) to propose an explicit modeling of the mixing through additional terms in the fluid equations.”
THE GENESIS OF THE MILKY WAY'S THICK DISK VIA STELLAR MIGRATION (2010, methodology): “Metal diffusion is calculated from a subgrid model of eddy turbulence based on the local smoothing length and velocity gradients (Smagorinsky 1963; Wadsley et al. 2008).”
Phantom: A Smoothed Particle Hydrodynamics and Magnetohydrodynamics Code for Astrophysics (2017, methodology): “In Phantom we use vusig = √ |Pa − Pb| ρab , (43) for simulations that do not involve self-gravity or external body forces (Price, 2008), and vusig = |vab · r̂ab|, (44) PASA (2018) doi:10.1017/pas.2018.xxx for simulations that do (Wadsley et al., 2008).”
NIHAO – IV: core creation and destruction in dark matter density profiles across cosmic time (2015, background): “The code includes a subgrid model for turbulent mixing of metals and energy (Wadsley et al. 2008), heating and cooling include photoelectric heating of dust grains, ultraviolet (UV) heating and ionization and cooling due to hydrogen, helium and metals (Shen et al. 2010).”
A new class of accurate, mesh-free hydrodynamic simulation methods (2014, background): “…the fluid (so it uniformly moves across the grid in an AMR code) substantially increases the errors and diffusion everywhere in the problem (see Wadsley et al. 2008; Tasker & Bryan 2008; Springel 2010); this can 3 It is sometimes said that “SPH does not converge,” or that “SPH is a…”
An improved SPH scheme for cosmological simulations (2015, background): “…entropy profiles to diverge towards the centres of dark matter haloes, at variance with Eulerian codes that predict entropy plateaus to build up (Frenk et al. 1999; Wadsley et al. 2008; Planelles & Quilis 2009; Vazza 2011; Power, Read & Hobbs 2014; Biffi & Valdarnini 2015; Rasia et al. 2015).”
The EAGLE simulations of galaxy formation: the importance of the hydrodynamics scheme (2015, background): “G A ] 1 6 rectly relevant the accretion of gas and satellite of galaxies (Frenk et al. 1999; Marri & White 2003; Okamoto et al. 2003; O’Shea et al. 2005; Agertz et al. 2007; Wadsley et al. 2008; Mitchell et al. 2009; Kereš et al. 2012; Sijacki et al. 2012).”
A test suite for quantitative comparison of hydrodynamic codes in astrophysics (2008, background): “In cosmological models, for instance, turbulence plays an important role as investigated by Wadsley et al. (2008) and Mitchell et al. (2008).”
Moving mesh cosmology: the hydrodynamics of galaxy formation (2011, methodology): “More generally, Wadsley et al. (2008) suggested that a physical modelling of heat diffusion is necessary when simulating high Reynolds number flows (both for SPH and mesh-based methods), and that by applying such an approach a flat entropy core is likely a more correct solution for non-radiative…”
NIHAO project – I. Reproducing the inefficiency of galaxy formation across cosmic time with a large sample of cosmological hydrodynamical simulations (2015, background): “Diffusion of quantities like metals and thermal energy between particles has been implemented as described in Wadsley et al. (2008).”