  The Kepler and TESS space missions significantly expanded our knowledge of
what types of stars display flaring activity by recording a vast amount of
super-flares from solar-like stars, as well as detecting flares from hotter
stars of A-F spectral types. Currently, we know that flaring occurs in the
stars as hot as B-type ones. However, the structures of atmospheres of hot B-A
stars crucially differ from the ones of late types, and thus the occurrence of
flaring in B-A type stars requires some extension of our theoretical views of
flare formation and therefore a detailed study of individual objects. Here we
present the results of our spectral and photometric study of HD 36030, which is
a B9 V star with flares detected by the TESS satellite. The spectra we acquired
suggest that the star is in a binary system with a low-mass secondary
component, but the light curve lacks any signs of periodic variability related
to orbital motion or surface magnetic fields. Because of that, we argue that
the flares originate due to magnetic interaction between the components of the
system.
