E pur si muove:Galilean-invariant cosmological hydrodynamical simulations on a moving mesh
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From gas to stars over cosmic time.A Lagrangian meshfree method applied to linear and nonlinear elasticityGalaxy formation with BECDM - I. Turbulence and relaxation of idealized haloes.Information field dynamics for simulation scheme construction.Rhapsody-G simulations – II. Baryonic growth and metal enrichment in massive galaxy clustersMass transfer and disc formation in AGB binary systemsAdaptive techniques for clustered N-body cosmological simulationsHow supernova feedback turns dark matter cusps into coresMapping substructure in the HST Frontier Fields cluster lenses and in cosmological simulationsSPH Methods in the Modelling of Compact ObjectsFormation and evolution of primordial protostellar systemsLessons from the Auriga discs: the hunt for the Milky Way's ex situ disc is not yet overMagnetic field formation in the Milky Way like disc galaxies of the Auriga projectOn the stellar halo metallicity profile of Milky Way-like galaxies in the Auriga simulationsThe Aquila comparison project: the effects of feedback and numerical methods on simulations of galaxy formationAGN-driven quenching of star formation: morphological and dynamical implications for early-type galaxiesnIFTy galaxy cluster simulations – V. Investigation of the cluster infall regionnIFTy galaxy cluster simulations – II. Radiative modelsnIFTy galaxy cluster simulations – IV. Quantifying the influence of baryons on halo propertiesnIFTY galaxy cluster simulations – III. The similarity and diversity of galaxies and subhaloesnIFTy galaxy cluster simulations – I. Dark matter and non-radiative modelsThe formation of entropy cores in non-radiative galaxy cluster simulations: smoothed particle hydrodynamics versus adaptive mesh refinementIntrinsic alignments of disc and elliptical galaxies in the MassiveBlack-II and Illustris simulationsThe formation of hot gaseous haloes around galaxiesSmall-scale galaxy clustering in the eagle simulationThe origin of the enhanced metallicity of satellite galaxiesThe eagle simulations of galaxy formation: the importance of the hydrodynamics schemeThe uniformity and time-invariance of the intra-cluster metal distribution in galaxy clusters from the IllustrisTNG simulationsSimulating galaxy formation with black hole driven thermal and kinetic feedback
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E pur si muove:Galilean-invariant cosmological hydrodynamical simulations on a moving mesh
description
im Januar 2010 veröffentlichter wissenschaftlicher Artikel
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wetenschappelijk artikel
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наукова стаття, опублікована в січні 2010
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name
E pur si muove:Galilean-invari ...... l simulations on a moving mesh
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E pur si muove:Galilean-invari ...... l simulations on a moving mesh
@nl
type
label
E pur si muove:Galilean-invari ...... l simulations on a moving mesh
@en
E pur si muove:Galilean-invari ...... l simulations on a moving mesh
@nl
prefLabel
E pur si muove:Galilean-invari ...... l simulations on a moving mesh
@en
E pur si muove:Galilean-invari ...... l simulations on a moving mesh
@nl
P1476
E pur si muove:Galilean-invari ...... l simulations on a moving mesh
@en
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10.1111/J.1365-2966.2009.15715.X
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P577
2010-01-11T00:00:00Z
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P818
P819
2010MNRAS.401..791S