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(Abridged) We study the kinematics of the dense gas in the Taurus L1495/B213filamentary region to investigate the mechanism of core formation. We useobservations of N2H+(1-0) and C18O(2-1) carried out with the IRAM 30mtelescope. We find that the dense cores in L1495/B213 are significantlyclustered in linear chain-like groups about 0.5pc long. The internal motions inthese chains are mostly subsonic and the velocity is continuous, indicatingthat turbulence dissipation in the cloud has occurred at the scale of thechains and not at the smaller scale of the individual cores. The chains alsopresent an approximately constant abundance of N2H+ and radial intensityprofiles that can be modeled with a density law that follows a softened powerlaw. A simple analysis of the spacing between the cores using an isothermalcylinder model indicates that the cores have likely formed by gravitationalfragmentation of velocity-coherent filaments. Combining our analysis of thecores with our previous study of the large-scale C18O emission from the cloud,we propose a two-step scenario of core formation in L1495/B213. In thisscenario, named "fray and fragment," L1495/B213 originated from the supersoniccollision of two flows. The collision produced a network of intertwinedsubsonic filaments or fibers ("fray" step). Some of these fibers accumulatedenough mass to become gravitationally unstable and fragment into chains ofclosely-spaced cores. This scenario may also apply to other regions of starformation.

Chains of dense cores in the Taurus L1495/B213 complex