Observations show gas in Mon R2 flows into the hub along filaments at higher rates than across them, with at least 30% of inter-filamentary mass potentially moving to filaments.
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astro-ph.GA 2years
2026 2verdicts
UNVERDICTED 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.
citing papers explorer
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From inter-filamentary gas to filaments and hubs: gas flows in the Mon R2 hub-filament system
Observations show gas in Mon R2 flows into the hub along filaments at higher rates than across them, with at least 30% of inter-filamentary mass potentially moving to filaments.
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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.