  Observed oscillations of coronal loops in EUV lines have been successfully
used to estimate plasma parameters in the inner corona (< 0.2 R_0, where R_0 is
the solar radius). However, coronal seismology in EUV lines fails for higher
altitudes because of rapid decrease in line intensity. We aim to use radio
observations to estimate the plasma parameters of the outer solar corona (> 0.2
R_0). We use the large Ukrainian radio telescope URAN-2 to observe type IV
radio burst at the frequency range of 8-32 MHz during the time interval of
09:50-12:30 UT in April 14, 2011. The burst was connected to C2.3 flare, which
occurred in AR 11190 during 09:38-09:49 UT. The dynamic spectrum of radio
emission shows clear quasi-periodic variations in the emission intensity at
almost all frequencies. Wavelet analysis at four different frequencies (29 MHz,
25 MHz, 22 MHz and 14 MHz) shows the quasi-periodic variation of emission
intensity with periods of 34 min and 23 min. The periodic variations can be
explained by the first and second harmonics of vertical kink oscillation of
transequatorial coronal loops, which were excited by the same flare. The apex
of transequatorial loops may reach up to 1.2 R_0 altitude. We derive and solve
the dispersion relation of trapped MHD oscillations in a longitudinally
inhomogeneous magnetic slab. The analysis shows that a thin (with width to
length ratio of 0.1), dense (with the ratio of internal and external densities
of > 20) magnetic slab with weak longitudinal inhomogeneity may trap the
observed oscillations. Seismologically estimated Alfv\'en speed inside the loop
at the height of 1 R_0 is 1000 km/s. Then the magnetic field strength at this
height is estimated as 0.9 G. Extrapolation of magnetic field strength to the
inner corona gives 10 G at the height of 0.1 R_0.
