  $\varepsilon$ Lupi A is a binary system consisting of two main sequence early
B-type stars Aa and Ab in a short period, moderately eccentric orbit. The close
binary pair is the only doubly-magnetic massive binary currently known. Using
photometric data from the BRITE-Constellation we identify a modest heartbeat
variation. Combining the photometry with radial velocities of both components
we determine a full orbital solution including empirical masses and radii.
These results are compared with stellar evolution models as well as
interferometry and the differences discussed. We also find additional
photometric variability at several frequencies, finding it unlikely these
frequencies can be caused by tidally excited oscillations. We do, however,
determine that these signals are consistent with gravity mode pulsations
typical for slowly pulsating B stars. Finally we discuss how the evolution of
this system will be affected by magnetism, determining that tidal interactions
will still be dominant.
