yt: A MULTI-CODE ANALYSIS TOOLKIT FOR ASTROPHYSICAL SIMULATION DATA

Turk, Matthew J.; Smith, Britton D.; Oishi, Jeffrey S.; Skory, Stephen; Skillman, Samuel W.; Abel, Tom; Norman, Michael L.

doi:10.1088/0067-0049/192/1/9

Cited by 1,227 publications

(891 citation statements)

References 38 publications

(48 reference statements)

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“…This results in a complicated shock morphology that is asymmetric on a large scale and on a small scale. This figure was produced using yt (Turk et al 2011). bounce, and then the spatially averaged neutrino evolution is smooth. Until ∼280 ms after bounce, there are only small differences between the neutrino luminosities in all models.…”

Section: Resultsmentioning

confidence: 99%

General-Relativistic Three-Dimensional Multi-Group Neutrino Radiation-Hydrodynamics Simulations of Core-Collapse Supernovae

Roberts

Ott

Haas

et al. 2016

ApJ

185

182

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We report on a set of long-term general-relativistic three-dimensional (3D) multi-group (energy-dependent) neutrino radiation-hydrodynamics simulations of core-collapse supernovae. We employ a full 3D two-moment scheme with the local M1 closure, three neutrino species, and 12 energy groups per species. With this, we follow the post-core-bounce evolution of the core of a nonrotating - M 27 progenitor in full unconstrained 3D and in octant symmetry for 380 ms. We find the development of an asymmetric runaway explosion in our unconstrained simulation. We test the resolution dependence of our results and, in agreement with previous work, find that low resolution artificially aids explosion and leads to an earlier runaway expansion of the shock. At low resolution, the octant and full 3D dynamics are qualitatively very similar, but at high resolution, only the full 3D simulation exhibits the onset of explosion.

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Section: Resultsmentioning

confidence: 99%

General-Relativistic Three-Dimensional Multi-Group Neutrino Radiation-Hydrodynamics Simulations of Core-Collapse Supernovae

Roberts

Ott

Haas

et al. 2016

ApJ

185

182

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“…The software used in this work was developed in part by the DOE NNSA ASC-and DOE Office of Science ASCR-supported Flash Center for Computational Science at the University of Chicago. The data analysis was partially carried out with the yt software (Turk et al 2011).…”

Section: Acknowledgementsmentioning

confidence: 99%

The turbulent life of dust grains in the supernova-driven, multiphase interstellar medium

Peters

Zhukovska

Naab

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Dust grains are an important component of the interstellar medium (ISM) of galaxies. We present the first direct measurement of the residence times of interstellar dust in the different ISM phases, and of the transition rates between these phases, in realistic hydrodynamical simulations of the multi-phase ISM. Our simulations include a timedependent chemical network that follows the abundances of H + , H, H 2 , C + and CO and take into account self-shielding by gas and dust using a tree-based radiation transfer method. Supernova explosions are injected either at random locations, at density peaks, or as a mixture of the two. For each simulation, we investigate how matter circulates between the ISM phases and find more sizeable transitions than considered in simple mass exchange schemes in the literature. The derived residence times in the ISM phases are characterised by broad distributions, in particular for the molecular, warm and hot medium. The most realistic simulations with random and mixed driving have median residence times in the molecular, cold, warm and hot phase around 17, 7, 44 and 1 Myr, respectively. The transition rates measured in the random driving run are in good agreement with observations of Ti gas-phase depletion in the warm and cold phases in a simple depletion model, although the depletion in the molecular phase is under-predicted. ISM phase definitions based on chemical abundance rather than temperature cuts are physically more meaningful, but lead to significantly different transition rates and residence times because there is no direct correspondence between the two definitions.

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“…The galaxy cluster halos were identified using a publicly available version of the HOP halo finding algorithm (Eisenstein & Hut, 1998) implemented in yt (Turk et al, 2011). In this paper, we use Rvir to define the virial radius of a galaxy cluster, such that the mean density inside this radius is 100 times the critical density of the universe at that redshift, consistent with the definitions in Bryan & Norman (1998 Colless & Dunn (1996a) 972 Table 1.…”

Section: Enzo Simulationmentioning

confidence: 99%

Warm gas in and around simulated galaxy clusters as probed by absorption lines

Emerick

Bryan

Putman

2015

Mon. Not. R. Astron. Soc.

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Understanding gas flows into and out of the most massive dark matter structures in our Universe, galaxy clusters, is fundamental to understanding their evolution. Gas in clusters is well studied in the hot (> 10 6 K) and cold (< 10 4 K) regimes, but the warm gas component (10 4 -10 6 K) is poorly constrained. It is challenging to observe directly, but can be probed through Lyα absorption studies. We produce the first systematic study of the warm gas content of galaxy clusters through synthetic Lyα absorption studies using cosmological simulations of two galaxy clusters produced with Enzo. We explore the spatial and kinematic properties of our cluster absorbers, and show that the majority of the identified absorbers are due to fast moving gas associated with cluster infall from IGM filaments. Towards the center of the clusters, however, the warm IGM filaments are no longer dominant and the absorbers tend to have higher column densities and metallicities, representing stripped galaxy material. We predict that the absorber velocity distribution should generally be bi-modal and discuss the effects of cluster size, mass, and morphology on the properties of the identified absorbers, and the overall cluster warm gas content. We find tentative evidence for a change in the well known increasing N HI with decreasing impact parameter for the most massive dark matter halos. Our results are compared directly to observations of Lyα absorbers in the Virgo cluster, and provide predictions for future Lyα absorption studies.

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yt: A MULTI-CODE ANALYSIS TOOLKIT FOR ASTROPHYSICAL SIMULATION DATA

Cited by 1,227 publications

References 38 publications

General-Relativistic Three-Dimensional Multi-Group Neutrino Radiation-Hydrodynamics Simulations of Core-Collapse Supernovae

General-Relativistic Three-Dimensional Multi-Group Neutrino Radiation-Hydrodynamics Simulations of Core-Collapse Supernovae

The turbulent life of dust grains in the supernova-driven, multiphase interstellar medium

Warm gas in and around simulated galaxy clusters as probed by absorption lines

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