  The interior physics of stars is currently not well constrained for
early-type stars. This is particularly pertinent for multiple systems as binary
interaction becomes more prevalent for more massive stars, which strongly
affects their evolution. High-precision photometry from the Transiting
Exoplanet Survey Satellite (TESS) mission offers the opportunity to remedy the
dearth of observations of pulsating stars that show evidence of binary
interaction, specifically pulsating mass-accreting components of semi-detached
Algol-type eclipsing binary (oEA) systems. We present the TESS light curve of
the circular eclipsing binary system U Gru (TIC 147201138), which shows
evidence for free heat-driven pressure modes and a series of tidally-perturbed
pressure modes. We highlight the asteroseismic potential of studying pulsating
stars in binary systems, and demonstrate how tidal asteroseismology can be
applied to infer the influence of binary interaction on stellar structure.
