  We present mapping results of two prestellar cores, L1544 and L694-2,
embedded in filamentary clouds in C$^{18}$O (3-2), $^{13}$CO (3-2), $^{12}$CO
(3-2), HCO$^+$ (4-3), and H$^{13}$CO$^+$ (4-3) with the JCMT telescope to
examine the role of the filamentary structures in the formation of dense cores
in the clouds, with new distance estimates for L1544 ($175_{-3}^{+4}$ pc) and
L694-2 ($203_{-7}^{+6}$ pc). From these observations, we found that the
non-thermal velocity dispersion of two prestellar cores and their surrounding
clouds are smaller than or comparable to the sound speed. This may indicate
that the turbulence has already been dissipated for both filaments and cores
during their formation time. We also found a $\lambda/4$ shift between the
periodic oscillations in the velocity and the column density distributions
implying the possible presence of gravitational core-forming flow motion along
the axis of the filament. The mass accretion rates due to these flow motions
are estimated to be 2-3 M$_\odot$ Myr$^{-1}$, being comparable to that for
Serpens cloud but much smaller than those for the Hub filaments, cluster, or
high mass forming filaments by 1 or 2 order of magnitudes. From this study, we
suggest that the filaments in our targets might be formed from the
shock-compression of colliding clouds, and then the cores are formed by
gravitational fragmentation of the filaments to evolve to the prestellar stage.
We conclude that the filamentary structures in the clouds play an important
role in the entire process of formation of dense cores and their evolution.
