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We investigate the formation and evolution of circumstellar disks inturbulent cloud cores until several 104 years after protostar formation usingsmoothed particle hydrodynamics (SPH) calculations. The formation and evolutionprocess of circumstellar disk in turbulent cloud cores differs substantiallyfrom that in rigidly rotating cloud cores. In turbulent cloud cores, afilamentary structure appears before the protostar formation and the protostarforms in the filament. If the turbulence is initially sufficiently strong, theremaining filament twists around the protostar and directly becomes arotation-supported disk. Upon formation, the disk orientation is generallymisaligned with the angular momentum of its host cloud core and it dynamicallyvaries during the main accretion phase, even though the turbulence is weak.This is because the angular momentum of the entire cloud core is mainlydetermined by the large scale velocity field whose wavelength is comparable tothe cloud scale, whereas the angular momentum of the disk is determined by thelocal velocity field where the protostar forms and these two velocity fields donot correlate with each other. In the case of disk evolution in a binary ormultiple stars, the disks are misaligned with each other at least during themain accretion phase, because there is no correlation between the velocityfields around the position where each protostar forms. In addition, each diskis also misaligned with the binary orbital plane. Such misalignment can explainthe recent observations of misaligned disks and misaligned protostellaroutflows.

Formation and Early Evolution of Circumstellar Disks in Turbulent Molecular Cloud Cores