  We present the results from 135 hours of nearly continuous time series
photometry on the ``hybrid'' (H-rich) PG1159 variable star HS2324+3944,
obtained in August-September 1997. The power spectrum of the data shows several
frequencies (about 20 or more), concentrated in three narrow and very crowded
regions near 475, 390 and 950 microHz in decreasing amplitude order. Most (if
not all) of the peaks in the latter region are linear combinations of the
high-amplitude frequencies between 455 and 500 microHz. If we divide the data
set into two equal parts, the power spectra are different. This is probably due
to a not sufficiently long (and therefore not completely resolved) light curve;
nevertheless an alternative hypothesis of a single damped oscillator may not be
completely ruled out. If we adopt the first hypothesis, the high concentration
of peaks between 455 and 500 microHz suggests the presence of both l=1 and l=2
high-overtone nonradial g-modes. The insufficient frequency resolution of our
data does not allow to obtain definite precision asteroseismology results.
Nevertheless a spacing of the signals is observed, probably due to stellar
rotation with a period of 2.3 days. If the signal spacing was due to the
successive overtones, the period spacings would be equal to 18.8 (l=1) and 10.4
(l=2) s.
