Interpretation and diversity of exoplanetary material orbiting white dwarfs

TL;DR

This study analyzes metal-polluted white dwarfs to understand the composition and diversity of accreted exoplanetary material, revealing insights into planetary formation and differentiation processes.

Contribution

It introduces an improved method for comparing white dwarf photospheric abundances with solar system objects, accounting for errors and limitations in interpretation.

Findings

White dwarfs accrete rocky, volatile-poor asteroidal material.

One star shows evidence of mantle-like planetary debris.

Variations in elemental abundances suggest diverse formation conditions.

Abstract

Nine metal-polluted white dwarfs are observed with medium-resolution optical spectroscopy,where photospheric abundances are determined and interpreted through comparison against solar system objects. An improved method of making such comparisons is presented that overcomes potential weaknesses of prior analyses, with the numerous sources of error considered to highlight the limitations on interpretation. The stars are inferred to be accreting rocky, volatile-poor asteroidal materials with origins in differentiated bodies, in line with the consensus model. The most heavily polluted star in the sample has 14 metals detected, and appears to be accreting material from a rocky planetesimal, whose composition is mantle-like with a small Fe-Ni core component. Some unusual abundances are present: one star is strongly depleted in Ca, while two others show Na abundances elevated above bulk Earth, speculated either to reflect diversity in the formation conditions of the source material, or to be traces of past accretion events. Another star shows clear signs that accretion ceased around 5 Myr ago,causing Mg to dominate the photospheric abundances, as it has the longest diffusion time of the observed elements. Observing such post-accretion systems allows constraints to be placed on models of the accretion process.