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Aims. To study intensity oscillations in the solar chromosphere/corona abovea quiet-Sun magnetic network. Methods. We analyse the time series of He II256.32, Fe XI 188.23 and Fe XII 195.12 spectral lines observed by EUV ImagingSpectrometer (EIS) on board Hinode near the south pole. Then we use a standardwavelet tool to produce power spectra of intensity oscillations above themagnetic network. Results. We get ~7 min intensity oscillations in all spectrallines and ~13 min intensity oscillations only in He II with the probability of~96-98 %, which probably reflects the process of magneto-acoustic wavepropagation above the network. Conclusions. We suggest that field-free cavityareas under bipolar magnetic canopies in the vicinity of magnetic network mayserve as resonators for the magneto-acoustic waves. The cavities withphotospheric sound speed and granular dimensions may produce the waves with theobserved periods. The waves may propagate upwards in the transitionregion/corona and cause observed intensity oscillations.

Intensity oscillations observed with Hinode near the south pole of the Sun: leakage of low frequency magneto-acoustic waves into the solar corona