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The new photometric data on pulsating Ap star HD~27463 obtained recently withthe Transiting Exoplanet Survey Satellite (\textit{TESS}) are analysed tosearch for variability. Our analysis shows that HD~27463 exhibits two types ofphotometric variability. The low frequency variability with the period $P$=~2.834274 $\pm$ 0.8 d can be explained in terms of axial stellar rotationassuming the oblique magnetic rotator model and presence of surfaceabundance/brightness spots, while the detected high-frequency variations arecharacteristics of $\delta$~Scuti pulsations. From the analysis of Balmer lineprofiles visible in two FEROS spectra of HD~27463 we have derived its effectivetemperature and surface gravity, finding values that are close to thosepublished for this star in the \textit{TESS} Input Catalogue (TIC). Knowing therotation period and the v$\sin{i}$ value estimated from the fitting of Balmerline profiles we found that the rotational axis is inclined to the line ofsight with an angle of $i=33\pm8\deg$. Our best-fitting model of the observedpulsation modes results in an overshoot parameter value $f_{ov} = 0.014$ andvalues of global stellar parameters that are in good agreement with the datareported in the TIC and with the data derived from fitting Balmer lineprofiles. This model indicates an age of 5.0 $\pm$~0.4 $\times 10^8$~yrs, whichcorresponds to a core hydrogen fraction of 0.33.

Rotational and pulsational variability in the TESS light curve of HD27463