  The new photometric data on pulsating Ap star HD~27463 obtained recently with
the Transiting Exoplanet Survey Satellite (\textit{TESS}) are analysed to
search for variability. Our analysis shows that HD~27463 exhibits two types of
photometric variability. The low frequency variability with the period $P$
=~2.834274 $\pm$ 0.000008 d can be explained in terms of axial stellar rotation
assuming the oblique magnetic rotator model and presence of surface
abundance/brightness spots, while the detected high-frequency variations are
characteristics of $\delta$~Scuti pulsations. From the analysis of Balmer line
profiles visible in two FEROS spectra of HD~27463 we have derived its effective
temperature and surface gravity, finding values that are close to those
published for this star in the \textit{TESS} Input Catalogue (TIC). Knowing the
rotation period and the v$\sin{i}$ value estimated from the fitting of Balmer
line profiles we found that the rotational axis is inclined to the line of
sight with an angle of $i=33\pm8\deg$. Our best-fitting model of the observed
pulsation modes results in an overshoot parameter value $f_{ov} = 0.014$ and
values of global stellar parameters that are in good agreement with the data
reported in the TIC and with the data derived from fitting Balmer line
profiles. This model indicates an age of 5.0 $\pm$~0.4 $\times 10^8$~yrs, which
corresponds to a core hydrogen fraction of 0.33.
