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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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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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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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.