ArkenstoneBH is a new subgrid model for the hot phase of black hole feedback that, in isolated galaxy tests, suppresses star formation by counteracting gas inflows from the circumgalactic medium.
Supernova feedback in numerical simulations of galaxy formation: separating physics from numerics
5 Pith papers cite this work. Polarity classification is still indexing.
5
Pith papers citing it
verdicts
UNVERDICTED 5representative citing papers
Deep learning identifies voids in NGC 628 with low association to known star clusters, supporting an evolutionary sequence from molecular clouds via stellar feedback to detached voids.
Simulations of an NGC 300-like galaxy find exponential distributions of feedback-driven bubble lifetimes and sizes that increase with galactocentric radius, plus matching Hα predictions.
N-body simulations show massive stars in TCCA clusters rapidly acquire triple or higher multiples and local density enhancements via dynamics, with multiplicity trends and shallower N_* profiles than competitive accretion models, matching AFGL 5180 better.
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
-
ArkenstoneBH. A model for high-specific energy black hole feedback in cosmological simulations
ArkenstoneBH is a new subgrid model for the hot phase of black hole feedback that, in isolated galaxy tests, suppresses star formation by counteracting gas inflows from the circumgalactic medium.
-
Automated void identification by Blendmask: from hierarchical molecular gas to hierarchical voids in NGC 628
Deep learning identifies voids in NGC 628 with low association to known star clusters, supporting an evolutionary sequence from molecular clouds via stellar feedback to detached voids.
-
Unmasking Stellar Feedback-Driven Bubbles: Identification and Properties Analysis
Simulations of an NGC 300-like galaxy find exponential distributions of feedback-driven bubble lifetimes and sizes that increase with galactocentric radius, plus matching Hα predictions.
-
Star cluster formation from turbulent clumps. V. Stellar clustering around massive stars
N-body simulations show massive stars in TCCA clusters rapidly acquire triple or higher multiples and local density enhancements via dynamics, with multiplicity trends and shallower N_* profiles than competitive accretion models, matching AFGL 5180 better.
-
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.