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Observations have revealed a large variety of structures (global asymmetries,warps, belts, rings) and dynamical phenomena ("falling-evaporating bodies" orFEBs, the "Beta Pic dust stream") in the disc of Beta Pictoris, most of whichmay indicate the presence of one or more planets orbiting the star. Becauseplanets of Beta Pic have not been detected by observations yet, we usedynamical simulations to find "numerical evidence" for a planetary system. Weshow that already one planet at 12 AU with a mass of 2 to 5 Mjup and aneccentricity 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 existenceof at least two additional planets at about 25 AU and 45 AU from the star seemslikely. We find rather strong upper limits of 0.6 Mjup and 0.2 Mjup on themasses of those planets. The same planets could, in principle, also account forthe outer rings observed at 500 - 800 AU.Comment: to appear in A&

Planets ofβ Pictoris revisited