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 ( \gtrsim 100 km/s ) is dictated by the initial ion skin depth while the amplification of the flow depends on local \beta .
It is shown , for the first time , that distances over which the flows become ” fast ” are \sim 0.01 R _ { s } from the interaction surface ; later the fast flow localizes ( with dimensions \lesssim 0.05 R _ { S } ) in the upper central region of the original arcade .
For fixed initial temperature the final speed ( \gtrsim 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 .