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The angular momentum of a molecular cloud core plays a key role in starformation, since it is directly related to the outflow and the jet emanatingfrom the new-born star and it eventually results in the formation of theprotoplanetary disk. However, the origin of the core rotation and its timeevolution are not well understood. Recent observations reveal that molecularclouds exhibit a ubiquity of filamentary structures and that star forming coresare associated with the densest filaments. Since these results suggest thatdense cores form primarily in filaments, the mechanism of core formation fromfilament fragmentation should explain the distribution of the angular momentumof these cores. In this paper we analyze the relation between velocityfluctuations along the filament close to equilibrium and the angular momentumof the cores formed along its crest. We first find that an isotropic velocityfluctuation that follows the three-dimensional Kolmogorov spectrum does notreproduce the observed angular momentum of molecular cloud cores. We thenidentify the need for a large power at small scales and study the effect ofthree power spectrum models. We show that the one-dimensional Kolmogorov powerspectrum with a slope -5/3 and an anisotropic model with reasonable parametersare compatible with the observations. Our results stress the importance of moredetailed and systematic observations of both the velocity structure alongfilaments and the angular momentum distribution of molecular cloud cores todetermine the validity of the mechanism of core formation from filamentarymolecular clouds.

An Origin for the Angular Momentum of Molecular Cloud Cores: a Prediction from Filament Fragmentation