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The HR8799 planetary system with four ~10 mJup planets in wide orbits up to70 au, and periods up to 500 yr has been detected with the direct imaging. Itsintriguing orbital architecture is not fully resolved due to time-limitedastrometry covering ~20 years. Earlier, we constructed a heuristic model of thesystem based on rapid, convergent migration of the planets. We developed abetter structured and CPU-efficient variant of this model. We re-analyzed theself-consistent, homogeneous astrometric dataset in Konopacky (2016). Thebest-fitting configuration agrees with our earlier findings. The planets arelikely involved in dynamically robust Laplace resonance chain. Hypotheticalplanets with masses below the current detection limit of 0.1-3 Jupiter masses,within the observed inner, or beyond the outer orbit, respectively, do notinfluence the long term stability of the system. We predict positions of suchnon-detected objects. The long-term stable orbital model of the observedplanets helps to simulate the dynamical structure of debris disks in thesystem. A CPU-efficient fast indicator technique makes it possible to revealtheir complex, resonant shape in 10^6 particles scale. We examine the inneredge of the outer disk detected between 90-145 au. We also reconstruct theouter disk assuming that it has been influenced by convergent migration of theplanets. A complex shape of the disk strongly depends on various dynamicalfactors, like orbits and masses of non-detected planets. It may be highlynon-circular and its models are yet non-unique, regarding both observationalconstraints, as well as its origin.

The orbital architecture and debris disks of the HR 8799 planetary system