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The evolution of a vacuum component of the Universe is investigated in thequantum as well as the classical regimes. Probably our Universe has arisen as avacuum fluctuation and very probably that it has had a high symmetry forPlanckian parameters. Besides, vacuum energy density has to be a positive one.In the early epochs during its cooling the Universe had been losing the highsymmetry by phase transitions since condensates of quantum fields carriednegative contributions (78 orders) to its positive energy density. It was theperiod of the Universe evolution during the first parts of the first second ofits life. After the last phase transition (quark-hadron) the vacuum energy `hashardened'. In this moment its energy density can be calculated using theZeldovich's formula inserting an average value of the pseudo-Goldstone bosonmasses (pi-mesons) that characterizes this chromodynamical vacuum. The chiralsymmetry was then lost. Dynamics of the equilibrium vacuum after its `hardness'is considered by applying the holographic conception. In this case the Universehas been losing vacuum energy (45 orders) on organization of new quantum statesduring 13.76 x 10^9 years. Using this conception we can get solution of thecosmological constant problem. 123 crisis orders problem may be resolved. Thedensity of vacuum energy cannot have a constant value in principle because ofthe new quantum states are organized during expansion of the Universe but theequation of state vacuum w= - 1 should be naturally constant. The density ofvacuum energy from z=0 up to z=10^11 is also calculated in the classical regimeof the Universe evolution.

A vacuum component of the Universe must evolve