Cosmic ray transport in molecular cloud simulations boosts star formation efficiency by up to 43% and yields a top-heavier IMF with a high-mass slope shallower by ~20%.
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Li PS, Klein RI, McKee CF
12 Pith papers cite this work. Polarity classification is still indexing.
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D-CAF simulations show that ongoing gas collapse during star formation shortens stellar crossing times, rendering gas expulsion more adiabatic and thereby regulating the survival and expansion rates of young stellar systems.
Lyα radiation pressure mildly reduces gas-to-star conversion efficiency in dense high-redshift clusters while dominating the launch of rapid outflows.
A new scale-aware diagnostic framework shows that unconstrained diffusion generative models exhibit structural freezing and instability instead of smooth physical responses under multiscale perturbations.
ALMA CO observations of NGC 4565 reveal a thin non-flaring molecular disk with a central gap, consistent GMC properties to 17 kpc, and a prominent star-forming ring feature.
Bursty stellar feedback produces systematically flatter metallicity gradients than smooth feedback in high-redshift galaxies across multiple simulation suites.
SED fitting of star clusters in NGC 628 identifies an evolutionary sequence from embedded young clusters to visible ones with a photo-dissociation region clearing timescale of approximately 4 Myr.
Kpc-resolution ALMA CO and dust maps of three z~3 dusty galaxies are consistent with gravo-turbulent star-formation models rather than non-turbulent predictions.
MST analysis of CMZoom data finds mass segregation in 5 of 17 CMZ clouds, inverse segregation or none in the rest, and no clear link to evolutionary stage or star-formation activity.
Multi-wavelength observations identify a compact hub-filament system in G286.21+0.17 whose core properties follow steep radial power laws consistent with competitive accretion.
Four controlled identical realizations of a galaxy-cluster zoom-in simulation reveal 10-25% variability in galaxy masses driven by stochastic processes and modulated by feedback, establishing a noise-dominated but statistically reproducible regime at low resolution.
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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Gauging the Impact of Cosmic Ray Feedback on the Stellar Initial Mass Function
Cosmic ray transport in molecular cloud simulations boosts star formation efficiency by up to 43% and yields a top-heavier IMF with a high-mass slope shallower by ~20%.
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Dynamical Cluster Assembly Framework (D-CAF): The Link Between Star Cluster Formation and Expansion Rates
D-CAF simulations show that ongoing gas collapse during star formation shortens stellar crossing times, rendering gas expulsion more adiabatic and thereby regulating the survival and expansion rates of young stellar systems.
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Lyman-alpha Radiation Pressure in Dense Star Clusters: Implications for Star Formation and Winds at Cosmic Dawn
Lyα radiation pressure mildly reduces gas-to-star conversion efficiency in dense high-redshift clusters while dominating the launch of rapid outflows.
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Scale-Aware Adversarial Analysis: A Diagnostic for Generative AI in Multiscale Complex Systems
A new scale-aware diagnostic framework shows that unconstrained diffusion generative models exhibit structural freezing and instability instead of smooth physical responses under multiscale perturbations.
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The Radial and Vertical Structure of Molecular Gas in the Edge-On Galaxy NGC 4565
ALMA CO observations of NGC 4565 reveal a thin non-flaring molecular disk with a central gap, consistent GMC properties to 17 kpc, and a prominent star-forming ring feature.
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Metallicity Gradients in Modern Cosmological Simulations II: The Role of Bursty Versus Smooth Feedback at High-Redshift
Bursty stellar feedback produces systematically flatter metallicity gradients than smooth feedback in high-redshift galaxies across multiple simulation suites.
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Feedback in Extragalactic Star Clusters (FEAST): Spectral Energy Distributions and the Physical Properties of Star Clusters in NGC 628 with CIGALE
SED fitting of star clusters in NGC 628 identifies an evolutionary sequence from embedded young clusters to visible ones with a photo-dissociation region clearing timescale of approximately 4 Myr.
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Investigating the role of turbulence in the interstellar medium in $z\sim3$ dusty star-forming galaxies using kpc-resolution ALMA dust and gas maps
Kpc-resolution ALMA CO and dust maps of three z~3 dusty galaxies are consistent with gravo-turbulent star-formation models rather than non-turbulent predictions.
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Mass Segregation in the CMZoom Survey
MST analysis of CMZoom data finds mass segregation in 5 of 17 CMZ clouds, inverse segregation or none in the rest, and no clear link to evolutionary stage or star-formation activity.
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Discovery of a Compact Hub-Filament System in G286.21+0.17 with JWST and ALMA: Insights into Protocluster Formation and Competitive Accretion
Multi-wavelength observations identify a compact hub-filament system in G286.21+0.17 whose core properties follow steep radial power laws consistent with competitive accretion.
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Variability in Cosmological Hydrodynamical Simulations: how Stochastic Processes, Numerical Effects, and Reproducibility Limits impact Predictability
Four controlled identical realizations of a galaxy-cluster zoom-in simulation reveal 10-25% variability in galaxy masses driven by stochastic processes and modulated by feedback, establishing a noise-dominated but statistically reproducible regime at low resolution.
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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.