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We point out a weak side of the commonly used determination of scalarcosmological perturbations lying in the fact that their average values can benonzero for some matter distributions. It is shown that introduction of thefinite-range gravitational potential instead of the infinite-range one resolvesthis problem. The concrete illustrative density profile is investigated indetail in this connection.

Zero average values of cosmological perturbations as an indispensable condition for the theory and simulations