  Molecular clouds are sites of star formation. Magnetic fields are believed to
play an important role in their dynamics and shaping morphology. We aim to
study any possible correlation that might exist between the magnetic fields
orientation inside the clouds and the magnetic fields at envelope scales and
their connection with respect to the observed morphology of the selected
clouds. We examine the magnetic field orientation towards the clouds L1512,
L1523, L1333, L1521E, L1544, L1517, L1780, and L183 using optical and
\textit{Planck} polarization observations. We also found the correlation
between the ambient magnetic field and core orientations derived using
\textit{Astrodendrogram} on the \textit{Herschel} 250 $\mu$m data. We find that
the magnetic fields derived from optical and \textit{Planck} agree with each
other. The derived magnetic fields are aligned along the observed emission of
each cloud as seen in \textit{Herschel} 250 $\mu$m data. We also find that the
relative orientation between the cores and the magnetic fields is random. This
lack of correlation may arise due to the fact that the core orientation could
also be influenced by the different magnetization within individual clouds at
higher densities or the feedback effects which may vary from cloud to cloud.
The estimated magnetic field strength and the mass-to-flux ratio suggest that
all the clouds are in a magnetically critical state except L1333, L1521E, and
L183 where the cloud envelope could be strongly supported by the magnetic field
lines.
