Within the framework of a two-fluid description possible pathways for the generation of fast flows (dynamical as well as steady) in the lower solar atmosphere is established. It is shown that a primary plasma flow (locally sub-Alfvénic) is accelerated when interacting with emerging/ambient arcade-like closed field structures. The acceleration implies a conversion of thermal and field energies to kinetic energy of the flow. The time-scale for creating reasonably fast flows ( 100 km/s) is dictated by the initial ion skin depth while the amplification of the flow depends on local β. It is shown, for the first time, that distances over which the flows become "fast" are ∼ 0.01 R s from the interaction surface; later the fast flow localizes (with dimensions 0.05 R S ) in the upper central region of the original arcade. For fixed initial temperature the final speed ( 500 km/s) of the accelerated flow, and the modification of the field structure are independent of the time-duration (life-time) of the initial flow. In the presence of dissipation, these flows are likely to play a fundamental role in the heating of the finely structured Solar atmosphere.