  Turbulence and magnetic fields are expected to be important for regulating
molecular cloud formation and evolution. However, their effects on subparsec to
100 parsec scales, leading to the formation of starless cores, is not well
understood. We investigate the prestellar core structure morphologies obtained
from analysis of the Herschel-SPIRE 350 $\mu$m maps of the Lupus I cloud. This
distribution is first compared on a statistical basis to the large scale shape
of the main filament. We find the distribution of the elongation position angle
of the cores to be consistent with a random distribution, which means no
specific orientation of the morphology of the cores is observed with respect to
a large-scale filament shape model for Lupus I, or relative to a large-scale
bent filament model. This distribution is also compared to the mean orientation
of the large-scale magnetic fields probed at 350 $\mu$m with the Balloon-borne
Large Aperture Telescope for Polarimetry (BLASTPol) during its 2010 campaign.
Here again we do not find any correlation between the core morphology
distribution and the average orientation of the magnetic fields on parsec
scales. Our main conclusion is that the local filament dynamics - including
secondary filaments that often run orthogonally to the primary filament - and
possibly small-scale variations in the local magnetic field direction, could be
the dominant factors for explaining the final orientation of each core.
