  From the Fourier analysis of the catalogue of ~200,000 variable candidates in
the OGLE-II Galactic fields, we found a sample of about 230 short-period
low-amplitude variable stars. From their position in the colour-magnitude
diagram and the observed periods (multiple in most cases), we identify the
stars as a mixture of Beta Cephei and Delta Scuti stars. Beta Cephei stars from
this sample are located in the Galactic disk at distances from 3 to 6 kpc. Many
of them shows large range of the excited periods, an indication of high
metallicity. We estimate that even a half of the sample of 230 short-period
variables we found, can be Beta Cephei stars. The periods alone, however, are
rarely sufficient to distinguish between both types of pulsators. We point out,
how this can be done observationally.
