  We present TESS photometry of the triple star system V1031 Ori (AB)C, which
exhibits short-period oscillations superimposed on an eclipsing light curve.
The high-quality data were analyzed in detail and combined with the published
spectroscopic measurements to obtain the fundamental stellar parameters of the
program target. The masses and radii of the eclipsing pair (AB) were determined
to about 0.5 \% and 0.7 \% precision, respectively. We found 23 significant
frequencies in two ranges of $<$ 2 day$^{-1}$ and 10.9$-$12.7 day$^{-1}$ from
the eclipse-subtracted residuals. Among them, sixteen in the gravity ($g$)-mode
region may be aliases and artefacts due to imperfect removal of the systematic
trends and the binary effects from the TESS data. Seven frequencies in the
pressure ($p$)-mode region were separated by the orbital frequency and split by
the average offset of 0.042 $\pm$ 0.003 day$^{-1}$ from their adjacent
harmonics. Further, the pulsation amplitudes are clearly modulated with the
binary star orbit. The results indicate that the $p$-mode frequencies are
tidally perturbed pulsations from the secondary component and the pulsation
axis could be aligned with the tidal axis.
