  Using the archival ROSAT observation of TT Ari, X-ray energy spectra in
different orbital phases and power spectra of the intensity time series are
presented. Spectral fits show that the source gets brighter during the
observation. The orbital modulation of the X-ray counting rate and
bremsstrahlung temperature suggests that soft X-ray emission peaks in the
orbital phase interval 0.75-0.90, when an outer disk hot spot is near the line
of sight. This correlates with the orbital modulation of C IV($\lambda$1549)
absorption. Timing analysis indicates that while the source gets brighter, the
frequency of the 1mHz oscillation is not correlated with X-ray intensity. This
implies that in the X-rays from TT Ari, the beat frequency model is not
appropriate for explaining the changes in the 1mHz oscillations.
  \keywords{Accretion discs - stars: TT Ari - stars: cataclysmic variables -
X-ray: binaries - X-rays
