Evolution of density and velocity profiles of dark matter and dark
  energy in spherical voids
  We analyse the evolution of cosmological perturbations which leads to the
formation of large isolated voids in the Universe. We assume that initial
perturbations are spherical and all components of the Universe (radiation,
matter and dark energy) are continuous media with perfect fluid
energy--momentum tensors, which interact only gravitationally. Equations of the
evolution of perturbations for every component in the comoving to cosmological
background reference frame are obtained from equations of energy and momentum
conservation and Einstein's ones and are integrated numerically. Initial
conditions are set at the early stage of evolution in the radiation-dominated
epoch, 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 energy
are formed and how they depend on parameters of dark energy and initial
conditions. In particular, it is shown that final matter density and velocity
amplitudes change within range $\sim$4-7\% when the value of equation-of-state
parameter of dark energy $w$ vary in the range from --0.8 to --1.2, and change
within $\sim$1\% only when the value of effective sound speed of dark energy
vary over all allowable range of its values.
