  We draw attention to the bright galaxies that do not show a bar in their
structure but have a flocculent spiral structure. Using the THINGS' and
HERACLES' kinematic data for four barless galaxies (NGC~2841, NGC~3512,
NGC~5055, NGC~7331) we built their mass models including dark halos. We
concluded that the fraction of the dark matter does not exceed 50\% within the
optical radii of the galaxies. This is too little to explain the lack of a bar
in these galaxies. In an attempt to understand the featureless structure of
these galaxies we constructed several $N$-body models with an initially reduced
content of dark matter. We concluded that, in addition to the low mass of the
dark halo, the decisive factor that leads to a barless disc is the start from
an initially unstable state. An isolated dynamically cold disc (with the Toomre
parameter $Q < 0.5$) settled into rotational equilibrium passes trough the
short stage of violent instability with fragmentation and formation of stellar
clumps. After that, it evolves passively and ends up with a featureless
structure. We assume that the barless flocculent galaxies studied in the
present work may be descendants of galaxies at high redshifts with rotation
curves which are consistent with the high mass fraction of baryons relative to
the total dark matter halo.
