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We calculate the nucleon parameters in symmetric nuclear matter employing theQCD sum rules approach. We focus on the average energy per nucleon and studythe equilibrium states of the matter. We treat the matter as a relativisticsystem of interacting nucleons. Assuming the dependence of the nucleon mass onthe light quark mass $m_q$ to be more important than that of nucleoninteractions we find that the contribution of the relativistic nucleons to thescalar quark condensate can be expressed as that caused by free nucleons atrest multiplied by the density dependent factor $F(\rho)$. We demonstrate thatthere are no equilibrium states while we include only the condensates withdimension $d \leq 3$. There are equilibrium states if we include the lowestorder radiative corrections and the condensates with $d \leq 4$. They manifestthemselves for the nucleon sigma term $\sigma_N >60$ MeV. Including thecondensates with $ d \leq 6$ we find equilibrium states of nuclear matter for$\sigma_N> 41$ MeV. In all cases the equilibrium states are due to influence ofthe relativistic motion of the nucleons composing the matter on the scalarquark condensate.

Equilibrium of nuclear matter in QCD sum rules