Massive stars in the Milky Way form over Myr timescales that increase with final mass, inferred from joint LF fitting of compact HII regions and OB stars under the inertial-inflow model.
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UNVERDICTED 5representative citing papers
Synthetic Herschel observations from simulations yield 8832 filaments hosting 94% of clumps, with power-law mass and length distributions and a density relation qualitatively matching the Hi-GAL survey.
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.
Extended gamma-ray emission around Berkeley 59 is produced by cosmic rays accelerated in cluster winds colliding with ambient gas.
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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Compact HII Regions as Clocks of Massive-Star Formation: Evidence for Long Formation Timescales
Massive stars in the Milky Way form over Myr timescales that increase with final mass, inferred from joint LF fitting of compact HII regions and OB stars under the inertial-inflow model.
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From filaments to clumps: filament properties with synthetic Herschel observations
Synthetic Herschel observations from simulations yield 8832 filaments hosting 94% of clumps, with power-law mass and length distributions and a density relation qualitatively matching the Hi-GAL survey.
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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.
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Diffuse gamma-ray emissions around the stellar cluster Berkeley 59
Extended gamma-ray emission around Berkeley 59 is produced by cosmic rays accelerated in cluster winds colliding with ambient gas.
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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.