Lumina is a 500 cMpc radiation-hydrodynamic simulation predicting late, stellar-driven hydrogen reionization ending near z≈4.75 and AGN-driven helium reionization nearly complete by z=3.
TreeCol: a novel approach to estimating column densities in astrophysical simulations
4 Pith papers cite this work, alongside 212 external citations. Polarity classification is still indexing.
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Simulations show recombination-weighted clumping is systematically lower than density-based measures, density-only prescriptions overpredict rates by 1.29-1.84 depending on redshift, and a new phase-space clumping factor isolates thermal and ionization effects at fixed density.
The Lumina simulation shows that explicit light-cone integrations produce a CMB optical depth 7% higher than volume-weighted ionization histories, with the excess accumulating near redshift 8 and mass-weighted estimates capturing most of the difference.
Review of MHD numerical methods for star formation, covering discretization techniques, divergence-free constraints, sink particles, and non-ideal effects like diffusion and the Hall effect.
citing papers explorer
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Introducing the Lumina project: large-volume radiation-hydrodynamic simulations of the epochs of hydrogen and helium reionization
Lumina is a 500 cMpc radiation-hydrodynamic simulation predicting late, stellar-driven hydrogen reionization ending near z≈4.75 and AGN-driven helium reionization nearly complete by z=3.
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The Lumina Project: Intergalactic Clumping and Recombination Sinks
Simulations show recombination-weighted clumping is systematically lower than density-based measures, density-only prescriptions overpredict rates by 1.29-1.84 depending on redshift, and a new phase-space clumping factor isolates thermal and ionization effects at fixed density.
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The Lumina Project: CMB Optical Depth Fluctuations from Patchy Reionization
The Lumina simulation shows that explicit light-cone integrations produce a CMB optical depth 7% higher than volume-weighted ionization histories, with the excess accumulating near redshift 8 and mass-weighted estimates capturing most of the difference.
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Numerical Methods for Simulating Star Formation
Review of MHD numerical methods for star formation, covering discretization techniques, divergence-free constraints, sink particles, and non-ideal effects like diffusion and the Hall effect.