With the image of the Sun held fixed, time variations of solar magnetic field were recorded simultaneously in two lines (λ5250 and λ6103) with the aid of double magnetograph (for the description see Severny, 1966, examples of such records are on Figures 1 and 2). The resolution was 2″.5 × 4″.5. The records in both lines λ5250 and λ6103 covering a time interval of about 1 hour show oscillations with the period ∼7·4min and amplitudes 10–20 gauss for moderately active region (full lines on the top of Figure 2). The oscillations of the magnetic field at both levels (the heights of λ 5250 and λ6103 differ by 260 km) are sometimes synchronous but now and then phase shift appears. For quiet regions near the centre of the disk the oscillations with the period ∼ 9·0 min and amplitudes less than 5 gauss are recorded and presented in Figure 1 (full line). These 7–9 min oscillations are probably sometimes damped or interrupted by more short-period fluctuations (with the mean period 80s) of smaller amplitude, but these last oscillations could be due to the fluctuations of seeing.