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We make use of a new hybrid method to simulate the long-term, multiple-orbitdisc formation through tidal disruptions of rocky bodies by white dwarfs, athigh-resolution and realistic semi-major axis. We perform the largest-yet suiteof simulations for dwarf and terrestrial planets, spanning four orders ofmagnitude in mass, various pericentre distances and semi-major axes between 3AU and 150 AU. This large phase space of tidal disruption conditions has notbeen accessible through the use of previous codes. We analyse the statisticaland structural properties of the emerging debris discs, as well as the ejectedunbound debris contributing to the population of interstellar asteroids. Unlikeprevious tidal disruption studies of small asteroids which form ring-likestructures on the original orbit, we find that the tidal disruption of largerbodies usually forms dispersed structures of interlaced elliptic eccentricannuli on tighter orbits. We characterize the (typically power-law)size-distribution of the ejected interstellar bodies as well as theircomposition, rotation velocities and ejection velocities. We find them to besensitive to the depth (impact parameter) of the tidal disruption. Finally, webriefly discuss possible implications of our results in explaining the peculiarvariability of Tabby's star, the origin of the transit events of ZTF J0139+5245and the formation of a planetary core around SDSS J1228+1040.

Tidal disruption of planetary bodies by white dwarfs II: Debris disc structure and ejected interstellar asteroids