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Second-order power spectra of Cosmic Microwave Background (CMB) anisotropiesdue to random primordial perturbations at the matter dominant stage arestudied, based on the relativistic second-order theory of perturbations in flatcosmological models and on the second-order formula of CMB anisotropies derivedby Mollerach and Matarrese. So far the second-order integrated Sachs-Wolfeeffect has been analyzed using the three-point correlation or bispectrum. Inthis paper we derive the second-order term of power spectra given using thetwo-point correlation of temperature fluctuations.  The second-order density perturbations are small, compared with thefirst-order ones. The second-order power spectra of CMB anisotropies, however,are not small at all, compared with the first-order power spectra, because atthe early stage the first-order integrated Sachs-Wolfe effect is very small andthe second-order integrated Sachs-Wolfe effect may be dominant over thefirst-order ones. So their characteristic behaviors may be measured through thefuture precise observation and bring useful informations on the structure andevolution of our universe in the future.

Second-order power spectra of CMB anisotropies due to primordial random perturbations in flat cosmological models