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(Abridged) Aims. We intend to derive statistical properties of stochastic gasmotion inside the dense low mass star forming molecular cores traced byNH3(1,1) and (2,2) emission lines. Methods. We use the spatial two-pointautocorrelation (ACF) and structure functions calculated from maps of theradial velocity fields. Results. We find oscillating ACFs which eventuallydecay to zero with increasing lags on scales of 0.04 <= l <= 0.5 pc. Thecurrent paradigm supposes that the star formation process is controlled by theinterplay between gravitation and turbulence, the latter preventing molecularcores from a rapid collapse due to their own gravity. Thus, oscillating ACFsmay indicate a damping of the developed turbulent flows surrounding the densebut less turbulent core - a transition to dominating gravitational forces and,hence, to gravitational collapse.

Star-forming regions of the Aquila rift cloud complex. II. Turbulence in molecular cores probed by NH3 emission