  Exoplanet properties crucially depend on their host stars' parameters. In
case the exoplanet host star shows pulsations, asteroseismology can be used for
an improved description of the stellar parameters. 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. We conduct a frequency analysis using
three seasons of BRITE-Constellation observations in the BRITE blue and red
filters, the ~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. We identify 15 pulsation frequencies in the range from 34 to 55c/d,
where two display clear amplitude variability. We use the normalised amplitudes
in up to five passbands to identify the modes as three l = 1, six l = 2 and six
l = 3 modes. beta Pic is shown to be non-magnetic with an upper limit of the
possible undetected dipolar field of 300G. 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+-0.025Rsun, and a mass of 1.797+-0.035Msun. The ~2%
errors in radius and mass do not account for uncertainties in the models and a
potentially erroneous mode-identification.
