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Turbulence and magnetic fields are expected to be important for regulatingmolecular cloud formation and evolution. However, their effects on subparsec to100 parsec scales, leading to the formation of starless cores, is not wellunderstood. We investigate the prestellar core structure morphologies obtainedfrom analysis of the Herschel-SPIRE 350 $\mu$m maps of the Lupus I cloud. Thisdistribution is first compared on a statistical basis to the large scale shapeof the main filament. We find the distribution of the elongation position angleof the cores to be consistent with a random distribution, which means nospecific orientation of the morphology of the cores is observed with respect toa large-scale filament shape model for Lupus I, or relative to a large-scalebent filament model. This distribution is also compared to the mean orientationof the large-scale magnetic fields probed at 350 $\mu$m with the Balloon-borneLarge Aperture Telescope for Polarimetry (BLASTPol) during its 2010 campaign.Here again we do not find any correlation between the core morphologydistribution and the average orientation of the magnetic fields on parsecscales. Our main conclusion is that the local filament dynamics - includingsecondary filaments that often run orthogonally to the primary filament - andpossibly small-scale variations in the local magnetic field direction, could bethe dominant factors for explaining the final orientation of each core.

Comparison of Prestellar Core Elongations and Large-Scale Molecular Cloud Structures in the Lupus I Region