2025MNRAS.541..610L

Planetary material accreted by white dwarfs provides unique insights regarding exoplanetary composition. The evolutionary pathways of planetary bodies around white dwarfs are crucial to understanding the presence of close-in planetary material, observed in the form of pollutants in the atmospheres of white dwarfs and planetary material transiting white dwarfs. Periodic transits around white dwarfs potentially reveal the existence of close-in planetary bodies undergoing dust production. Tidal interactions can bring planetesimals that have been gravitationally perturbed on to long-period highly eccentric orbits around white dwarfs towards shorter orbital periods and smaller eccentricities. Tidal interactions may also induce melting and volcanism in these planetesimals, potentially being a mechanism for dust production, the result of which may be seen in transit. Tidally induced volcanism may be triggered in a wide parameter space: for a 100 km-sized rocky planetesimals perturbed to a pericentre distance $\lesssim 0.01\, \rm au$ ($\gtrsim$ twice its Roche limit), both on long-period ($\sim 100\, \rm d$) highly eccentric orbits and short-period ($\sim 10\, \rm h$) near circular orbits. We comment on the potential link between the resultant volcanic ejecta and observed optical transits.