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We analyse the evolution of cosmological perturbations which leads to theformation of large isolated voids in the Universe. We assume that initialperturbations are spherical and all components of the Universe (radiation,matter and dark energy) are continuous media with perfect fluidenergy--momentum tensors, which interact only gravitationally. Equations of theevolution of perturbations for every component in the comoving to cosmologicalbackground reference frame are obtained from equations of energy and momentumconservation and Einstein's ones and are integrated numerically. Initialconditions are set at the early stage of evolution in the radiation-dominatedepoch, when the scale of perturbation is much larger than the particle horizon.Results show how the profiles of density and velocity of matter and dark energyare formed and how they depend on parameters of dark energy and initialconditions. In particular, it is shown that final matter density and velocityamplitudes change within range $\sim$4-7\% when the value of equation-of-stateparameter of dark energy $w$ vary in the range from --0.8 to --1.2, and changewithin $\sim$1\% only when the value of effective sound speed of dark energyvary over all allowable range of its values.

Evolution of density and velocity profiles of dark matter and dark energy in spherical voids