Origin of the dense core mass function in contracting filaments

Abstract

Mass functions of starless dense cores (CMFs) may arise from contraction and dispersal of core-forming filaments. In an illustrative model, a filament contracts radially by self-gravity, increasing the mass of its cores. During this contraction, FUV photoevaporation and ablation by shocks and winds disperse filament gas and limit core growth. The stopping times of core growth are described by a waiting-time distribution. The initial filament column density profile and the resulting CMF each match recent Herschel observations in detail. Then low-mass cores have short growth ages and arise from the innermost filament gas, while massive cores have long growth ages and draw from more extended filament gas. The model fits the initial density profile and CMF best for mean core density 2 10^4 cm^-3 and filament dispersal time scale 0.5 Myr. Then the typical core mass, radius, mean column density, and contraction speed are respectively 0.8 solar masses, 0.06 pc, 6 10^21 cm^-2, and 0.07 km s^-1, also in accord with observed values.

to appear in The Astrophysical Journal

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• Cloud Structure of Galactic OB Cluster Forming Regions from Combining Ground and Space Based Bolometric Observations
• Role of $f(R,T,R_{\mu \nu }{T}^{\mu \nu })$ Model on the Stability of Cylindrical Stellar Model
• The fragmentation and stability of hierarchical structure in Serpens South
• Oscillations and stability of polytropic filaments
• An Ammonia Spectral Map of the L1495-B218 Filaments in the Taurus Molecular Cloud: II CCS & HC${}_7$N Chemistry and Three Modes of Star Formation in the Filaments
• Protostar mass functions in young clusters
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• Instability Analysis of Cylindrical Stellar Object in Brans-Dicke Gravity
• The Correlation of Dust and Gas Emission in Star-Forming Environments