  $\zeta$ Phoenicis is a bright binary system containing B6V and B8V stars. It
has deep total and annular eclipses, a slightly eccentric orbit with a period
of 1.669 d, apsidal motion and a third body on a wider orbit. The Transiting
Exoplanet Survey Satellite light curve and published radial velocities of this
system are analysed to determine masses of 3.91 +/- 0.06 Msun and 2.54 +/- 0.03
Msun and radii of 2.84 +/- 0.02 Rsun and 1.89 +/- 0.01 Rsun. The resulting
distance to the system is in agreement with its trigonometric parallax. The
physical properties of the stars, with the exception of the effective
temperature of the secondary component, can be matched by the predictions of
several sets of theoretical stellar evolutionary models for a solar chemical
composition and an age of 70 to 90 Myr. A spectroscopic analysis of this system
is encouraged for the determination of the photospheric chemical composition of
the stars, plus improved measurements of their masses and effective
temperatures.
