  We present an analysis of the high-mass eclipsing binary system VV Ori based
on photometry from the TESS satellite. The primary star (B1V, 9.5 Msun) shows
beta Cephei pulsations and the secondary (B7V, 3.8 Msun) is possibly a
slowly-pulsating B star. We detect 51 significant oscillation frequencies,
including two multiplets with separations equal to the orbital frequency,
indicating that the pulsations are tidally perturbed. We analyse the TESS light
curve and published radial velocities to determine the physical properties of
the system. Both stars are only the second of their pulsation type with a
precisely-measured mass. The orbital inclination is also currently decreasing,
likely due to gravitational interactions with a third body.
