  We analyse the evolution of cosmological perturbations which leads to the
formation of large voids in the distribution of galaxies. We assume that
perturbations are spherical and all components of the Universe - radiation,
matter and dark energy - are continuous media with ideal fluid energy-momentum
tensors, which interact only gravitationally. Equations of the evolution of
perturbations in the comoving to cosmological background reference frame for
every component are obtained from equations of conservation and Einstein's ones
and are integrated by modified Euler method. Initial conditions are set at the
early stage of evolution in the radiation-dominated epoch, when the scale of
perturbation is mush larger than the particle horizon. Results show how the
profiles of density and velocity of matter in spherical voids with different
overdensity shells are formed.
