Context : Exoplanet properties crucially depend on their host stars ’ parameters : more accurate stellar parameters yield more accurate exoplanet characteristics . In case the exoplanet host star shows pulsations , asteroseismology can be used for an improved description of the stellar parameters . Aims : We aim to revisit the pulsational properties of \beta Pic and identify its pulsation modes from normalised amplitudes in five different passbands . We also investigate the potential presence of a magnetic field . Methods : We conduct a frequency analysis using three seasons of BRITE-Constellation observations in the BRITE filters , the \sim 620-day long bRing light curve and the nearly 8-year long SMEI photometric time series . We calculate normalised amplitudes using all passbands including previously published values obtained from ASTEP observations . We investigate the magnetic properties of \beta Pic using spectropolarimetric observations conducted with the HARPSpol instrument . Using 2D rotating models , we fit the normalised amplitudes and frequencies through Monte Carlo Markov Chains . Results : We identify 15 pulsation frequencies in the range from 34 to 55 d ^ { -1 } , where two – F13 at 53.6917 d ^ { -1 } and F11 at 50.4921 d ^ { -1 } – display clear amplitude variability . We use the normalised amplitudes in up to five passbands to identify the modes as three \ell = 1 , six \ell = 2 and six \ell = 3 modes . \beta Pic is shown to be non-magnetic with an upper limit of the possible undetected dipolar field of 300 Gauss . Conclusions : Multiple fits to the frequencies and normalised amplitudes are obtained including one with a near equator-on inclination for \beta Pic , which corresponds to our expectations based on the orbital inclination of \beta Pic b and the orientation of the circumstellar disk . This solution leads to a rotation rate of 27 % of the Keplerian break-up velocity , a radius of 1.497 \pm 0.025 R _ { \odot } , and a mass of 1.797 \pm 0.035 M _ { \odot } . The \sim 2 % errors in radius and mass do not account for uncertainties in the models and a potentially erroneous mode-identification .