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The angular momentum of molecular cloud cores plays a key role in the starformation process. However, the evolution of the angular momentum of molecularcloud cores formed in magnetized molecular filaments is still unclear. In thispaper, we perform three-dimensional magnetohydrodynamics simulations to revealthe effect of the magnetic field on the evolution of the angular momentum ofmolecular cloud cores formed through filament fragmentation. As a result, wefind that the angular momentum decreases by 30% and 50% at the mass scale of1Msun in the case of weak and strong magnetic field, respectively. By analyzingthe torques exerted on fluid elements, we identify the magnetic tension as thedominant process for angular momentum transfer for mass scales < 3Msun for thestrong magnetic field case. This critical mass scale can be understoodsemi-analytically as the timescale of magnetic braking. We show that theanisotropy of the angular momentum transfer due to the presence of strongmagnetic field changes the resultant angular momentum of the core only by afactor of two. We also find that the distribution of the angle between therotation axis and the magnetic field does not show strong alignment even justbefore the first core formation. Our results also indicate that the variety ofthe angular momentum of the cores are inherited from the difference of thephase of the initial turbulent velocity field. The variety could contribute tothe diversity in size and other properties of protoplanetary disks recentlyreported by observations.

Evolution of the Angular Momentum of Molecular Cloud Cores in Magnetized Molecular Filaments