CARPP recovers seven core parameters from multi-band dust continuum via layered radiative transfer, achieving <20% average relative error under a stated noise-resolution criterion and classifying TMC-1C as near-critical Bonnor-Ebert and Ori2-2 as power-law collapsing.
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Galli D, Walmsley M, Gon c ¸alves J
15 Pith papers cite this work. Polarity classification is still indexing.
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In DNS of barotropic gravitational collapse with purely irrotational initial turbulence, vorticity is not produced by the collapse; it scales with the initial velocity amplitude and stays at the level of non-collapsing control runs.
Blue-asymmetric spectral lines appear in 50-60% of dense cores within massive dark clumps, showing that gravitational collapse operates at core scales from prestellar stages onward and supports hierarchical star formation.
Dedner's mixed divergence cleaning produces substantial artifacts for strongly localized magnetic fields or sudden timestep changes; constrained transport is more accurate, and some prior early-Universe amplification claims may be affected.
A model based on Chandrasekhar's 1951 time-invariant quantity quantitatively explains the Mach-number dependence of the density power spectrum slope in isothermal supersonic turbulence and demonstrates that the slope cannot reliably determine the Mach number.
Bayesian IMF-aware inference on NGC 1569 clusters yields correlations between cluster mass-function truncation mass, galactocentric distance, metallicity, and gas ionization state.
A mean-field magnetic polytrope model shows radiation pressure can unbind an n=3 polytrope when the central overpressure exceeds roughly 0.15 times a mass-dependent factor under small radial perturbations.
Cosmological hydrodynamical simulations predict that UV diversity in Little Red Dots encodes direct-collapse black hole ages via a rapid transition from BH- to stellar-dominated emission after ~30 Myr.
Observational study of MBM12 shows CO-to-H2 conversion factor near galactic average with density-dependent variations, high virial parameters decreasing at small scales, broken power-law mass-size relations indicating external pressure, and magnetic field orientation transition at N(H2) = 4.5e21 cm-
Oblique filament collisions lead to gravitational collapse of the compressed cloud when post-collision |gravitational energy| exceeds kinetic plus thermal plus magnetic energies, with lower angles and lower velocities favoring hub-filament formation.
ALMA Cycle 6 data on Aquila dense cores identifies two starless sources and scale-dependent increases in multiplicity, consistent with turbulent core collapse simulations predicting 1.19 starless detections.
SPH simulations of filament fragmentation indicate isotopic inhomogeneities from 1 pc filaments survive in cores at reduced levels and potentially reach circumstellar disks.
Simulations of collapsing cores find that ε_ff varies with core definition via density threshold, open vs closed boundaries, and initial density, with higher values in low-mass cores due to lower infall rates.
APEX 1.3 mm observations of RCW120 S2 detect COMs including CH3OH, CH3CHO, CH3OCHO and CH3OCH3, reveal a radially stratified envelope, and show modest abundance mismatches with hot-core chemical models attributed to unresolved filling factor.
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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CARPP: Parametric Radiative-Transfer Fitting of Molecular Cores from Dust Continuum Data
CARPP recovers seven core parameters from multi-band dust continuum via layered radiative transfer, achieving <20% average relative error under a stated noise-resolution criterion and classifying TMC-1C as near-critical Bonnor-Ebert and Ori2-2 as power-law collapsing.
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No evidence of vorticity production from irrotational turbulent gravitational collapse yet
In DNS of barotropic gravitational collapse with purely irrotational initial turbulence, vorticity is not produced by the collapse; it scales with the initial velocity amplitude and stays at the level of non-collapsing control runs.
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Global and Local Infall in the ASHES Sample (GLASHES). II. Asymmetric Line Profiles around Dense Cores in 70 $\mu$m Dark Massive Clumps
Blue-asymmetric spectral lines appear in 50-60% of dense cores within massive dark clumps, showing that gravitational collapse operates at core scales from prestellar stages onward and supports hierarchical star formation.
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Systematic Comparison between Constrained Transport and Mixed Divergence Cleaning Methods for Astrophysical Magnetohydrodynamic Simulations
Dedner's mixed divergence cleaning produces substantial artifacts for strongly localized magnetic fields or sudden timestep changes; constrained transport is more accurate, and some prior early-Universe amplification claims may be affected.
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The slope of the power spectrum of the density field in isothermal supersonic compressible turbulence
A model based on Chandrasekhar's 1951 time-invariant quantity quantitatively explains the Mach-number dependence of the density power spectrum slope in isothermal supersonic turbulence and demonstrates that the slope cannot reliably determine the Mach number.
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Getting to know the Stellar Clusters in NGC 1569: Bayesian inference of stellar cluster properties in a dwarf starburst galaxy
Bayesian IMF-aware inference on NGC 1569 clusters yields correlations between cluster mass-function truncation mass, galactocentric distance, metallicity, and gas ionization state.
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Non-linear Dynamical Stability of Magnetic Polytropes
A mean-field magnetic polytrope model shows radiation pressure can unbind an n=3 polytrope when the central overpressure exceeds roughly 0.15 times a mass-dependent factor under small radial perturbations.
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Ultraviolet diversity of Little Red Dots as a probe for direct-collapse black hole ages
Cosmological hydrodynamical simulations predict that UV diversity in Little Red Dots encodes direct-collapse black hole ages via a rapid transition from BH- to stellar-dominated emission after ~30 Myr.
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B-Fields and Star Formation across Scales with TRAO (B-FROST): CO Abundances, Dynamics and Relative Orientations in the Translucent High Latitude Cloud MBM12
Observational study of MBM12 shows CO-to-H2 conversion factor near galactic average with density-dependent variations, high virial parameters decreasing at small scales, broken power-law mass-size relations indicating external pressure, and magnetic field orientation transition at N(H2) = 4.5e21 cm-
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Evolution of compressed clouds formed by filament coalescence. I. Oblique collisions
Oblique filament collisions lead to gravitational collapse of the compressed cloud when post-collision |gravitational energy| exceeds kinetic plus thermal plus magnetic energies, with lower angles and lower velocities favoring hub-filament formation.
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Fragmentation in the Serpens/Aquila Star-forming Region
ALMA Cycle 6 data on Aquila dense cores identifies two starless sources and scale-dependent increases in multiplicity, consistent with turbulent core collapse simulations predicting 1.19 starless detections.
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Formation of Isotopically Heterogeneous Molecular Cloud Cores in Filamentary Molecular Clouds
SPH simulations of filament fragmentation indicate isotopic inhomogeneities from 1 pc filaments survive in cores at reduced levels and potentially reach circumstellar disks.
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The efficiency per free-fall time as a ratio of the Star Formation Rate to the gas-infall rate in collapsing cores: dependence on the core definition, accretion, and radial structure
Simulations of collapsing cores find that ε_ff varies with core definition via density threshold, open vs closed boundaries, and initial density, with higher values in low-mass cores due to lower infall rates.
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Complex organic molecules in the young hot core RCW 120 S2
APEX 1.3 mm observations of RCW120 S2 detect COMs including CH3OH, CH3CHO, CH3OCHO and CH3OCH3, reveal a radially stratified envelope, and show modest abundance mismatches with hot-core chemical models attributed to unresolved filling factor.
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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.