2016/07/01 by Adrian S. Hamers, Simon Portegies Zwart, Simon F. Portegies Zwart · 2 citations
Physics and Astronomy · #Accretion (finance) #Astro and Planetary Science #Astrobiology #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Physics #Planet #Stars #Stellar, planetary, and galactic studies #White dwarf #astro-ph.EP #astro-ph.SR
paper · pdf · doi:10.1093/mnrasl/slw134
Accepted for publication in MNRAS Letters. 5 pages, 5 figures
openalex publication_date 2016/07/01 · arxiv created 2016/07/05 · arxiv updated 2016/08/03 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract Approximately 0.2 ± 0.2 of white dwarfs (WDs) show signs of pollution by metals, which is likely due to the accretion of tidally disrupted planetary material. Models invoking planet–planet interactions after WD formation generally cannot explain pollution at cooling times of several Gyr. We consider a scenario in which a planet is perturbed by Lidov–Kozai oscillations induced by a binary companion and exacerbated by stellar mass-loss, explaining pollution at long cooling times. Our computed accretion rates are consistent with observations assuming planetary masses between ∼0.01 and 1 MMars, although non-gravitational effects may already be important for masses ≲0.3 MMars. The fraction of polluted WDs in our simulations, ∼0.05, is consistent with observations of WDs with intermediate cooling times between ∼0.1 and 1 Gyr. For cooling times ≲0.1 Gyr and ≳1 Gyr, our scenario cannot explain the high observed pollution fractions of up to 0.7. Nevertheless, our results motivate searches for companions around polluted WDs.