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.
hub
Galli D, Walmsley M, Gon c ¸alves J
14 Pith papers cite this work. Polarity classification is still indexing.
14
Pith papers citing it
hub tools
citation-role summary
background 2
citation-polarity summary
roles
background 2polarities
background 2representative citing papers
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.
Constrained transport outperforms Dedner's divergence cleaning in MHD simulations by avoiding spurious artifacts when magnetic fields are localized or timesteps vary suddenly.
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.
Direct numerical simulations find no vorticity generation attributable to the collapse flow itself when starting from irrotational turbulence in a barotropic, non-magnetized fluid.
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
-
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.