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Asteroid material is detected in white dwarfs (WDs) as atmospheric pollutionby metals, in the form of gas/dust discs, or in photometric transits. Withinthe current paradigm, minor bodies need to be scattered, most likely byplanets, into highly eccentric orbits where the material gets disrupted bytidal forces and then accreted onto the star. This can occur through aplanet-planet scattering process triggered by the stellar mass loss during thepost main-sequence evolution of planetary systems. So far, studies of the$N$-body dynamics of this process have used artificial planetary systemarchitectures built ad hoc. In this work, we attempt to go a step further andstudy the dynamical instability provided by more restrictive systems, that, atthe same time allow us an exploration of a wider parameter space: the hundredsof multiple planetary systems found around main-sequence (MS) stars. We findthat most of our simulated systems remain stable during the MS, Red andAsymptotic Giant Branch and for several Gyr into the WD phases of the hoststar. Overall, only $\approx$ 2.3$\%$ of the simulated systems lose a planet onthe WD as a result of dynamical instability. If the instabilities take placeduring the WD phase most of them result in planet ejections with just 5planetary configurations ending as a collision of a planet with the WD. Finally3.2$\%$ of the simulated systems experience some form of orbital scattering ororbit crossing that could contribute to the pollution at a sustained rate ifplanetesimals are present in the same system.

Dynamical evolution of two-planet systems and its connection with white dwarf atmospheric pollution