Sub-Alfvénic MHD simulations with projection effects reproduce the range of observed polarization (μ, σ) values in Orion ISF, showing these statistics alone cannot constrain the 3D Alfvén Mach number.
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A spectral-multigrid Poisson solver for spherical and cylindrical coordinates achieves second-order accuracy on uniform and logarithmic radial grids with vacuum boundary handling via screening mass and scales to 4096 cores.
Jet feedback in centrally concentrated clouds reduces star formation efficiency to 12-16% and yields cluster structures more consistent with observations than models without jets.
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.
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.
COLIBRE calibrates supernova and AGN feedback parameters in multi-phase ISM cosmological simulations using emulator-based fitting to reproduce the z=0 galaxy stellar mass function and size-stellar mass relation at three resolutions.
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.
citing papers explorer
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Projection Is All You Need: Interpreting Polarization Measurements in the Orion Clouds with Sub-Alfv\'enic MHD Simulations
Sub-Alfvénic MHD simulations with projection effects reproduce the range of observed polarization (μ, σ) values in Orion ISF, showing these statistics alone cannot constrain the 3D Alfvén Mach number.
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Centrally concentrated star formation in young clusters II: Jet feedback
Jet feedback in centrally concentrated clouds reduces star formation efficiency to 12-16% and yields cluster structures more consistent with observations than models without jets.
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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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COLIBRE: calibrating subgrid feedback in cosmological simulations that include a cold gas phase
COLIBRE calibrates supernova and AGN feedback parameters in multi-phase ISM cosmological simulations using emulator-based fitting to reproduce the z=0 galaxy stellar mass function and size-stellar mass relation at three resolutions.
- cuRAMSES: Scalable AMR Optimizations for Large-Scale Cosmological Simulations