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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4 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
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astro-ph.GA 4years
2026 4verdicts
UNVERDICTED 4representative citing papers
Simulations of the Aquila Rift show uneven clumps accreting gas and merging along filaments to form a fractal cluster whose velocity anisotropies, rotation, and expansion record the assembly history even after gas removal.
Synthetic Herschel observations from simulations yield 8832 filaments hosting 94% of clumps, with power-law mass and length distributions and a density relation qualitatively matching the Hi-GAL survey.
Observational study of G12.79+0.43 identifies YSOs and HII regions powered by B-type stars and associates the complex with the rim of a molecular superbubble of diameter ~50 pc and expansion age ~0.3 Myr without establishing causality.
citing papers explorer
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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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Simulating Star Formation and Star Cluster Assembly in the Aquila Rift Using Archival Observations
Simulations of the Aquila Rift show uneven clumps accreting gas and merging along filaments to form a fractal cluster whose velocity anisotropies, rotation, and expansion record the assembly history even after gas removal.
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From filaments to clumps: filament properties with synthetic Herschel observations
Synthetic Herschel observations from simulations yield 8832 filaments hosting 94% of clumps, with power-law mass and length distributions and a density relation qualitatively matching the Hi-GAL survey.
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Star Formation at the Periphery of a Molecular Superbubble: The Case of G12.79+0.43
Observational study of G12.79+0.43 identifies YSOs and HII regions powered by B-type stars and associates the complex with the rim of a molecular superbubble of diameter ~50 pc and expansion age ~0.3 Myr without establishing causality.