  Observations have revealed a large variety of structures (global asymmetries,
warps, belts, rings) and dynamical phenomena ("falling-evaporating bodies" or
FEBs, the "Beta Pic dust stream") in the disc of Beta Pictoris, most of which
may indicate the presence of one or more planets orbiting the star. Because
planets of Beta Pic have not been detected by observations yet, we use
dynamical simulations to find "numerical evidence" for a planetary system. We
show that already one planet at 12 AU with a mass of 2 to 5 Mjup and an
eccentricity smaller or equal 0.1 can probably account for three major features
(main warp, two inner belts, FEBs) observed in the Beta Pic disc. The existence
of at least two additional planets at about 25 AU and 45 AU from the star seems
likely. We find rather strong upper limits of 0.6 Mjup and 0.2 Mjup on the
masses of those planets. The same planets could, in principle, also account for
the outer rings observed at 500 - 800 AU.
