2014/09/08 by Dimitri Veras, Z. M. Leinhardt, Zoe M. Leinhardt +3 · 2 citations
Physics and Astronomy · #Asteroid #Asteroid belt #Astro and Planetary Science #Astrobiology #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Galaxy #Halo #Orbital eccentricity #Physics #Planetary system #Stars #Stellar, planetary, and galactic studies #White dwarf #astro-ph.EP #astro-ph.SR
paper · pdf · doi:10.1093/mnras/stu1871
Accepted for publication in MNRAS
arxiv created 2014/09/08 · openalex publication_date 2014/10/16 · arxiv updated 2015/06/22 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
25–50 per cent of all white dwarfs (WDs) host observable and dynamically active remnant planetary systems based on the presence of close-in circumstellar dust and gas and photospheric metal pollution. Currently accepted theoretical explanations for the origin of this matter include asteroids that survive the star's giant branch evolution at au-scale distances and are subsequently perturbed on to WD-grazing orbits following stellar mass-loss. In this work, we investigate the tidal disruption of these highly eccentric (e > 0.98) asteroids as they approach and tidally disrupt around the WD. We analytically compute the disruption time-scale and compare the result with fully self-consistent numerical simulations of rubble piles by using the N-body code pkdgrav. We find that this time-scale is highly dependent on the orbit's pericentre and largely independent of its semimajor axis. We establish that spherical asteroids readily break up and form highly eccentric collisionless rings, which do not accrete on to the WD without additional forces such as radiation or sublimation. This finding highlights the critical importance of such forces in the physics of WD planetary systems.