Rapid Formation of Exoplanetesimals Revealed by White Dwarfs

TL;DR

This paper presents observational evidence from white dwarf systems indicating that planetesimals form within the first few hundred thousand years after molecular cloud collapse, much earlier than previously thought, driven by short-lived radioactive heating.

Contribution

It provides new evidence that planetesimals form rapidly during star formation, supported by white dwarf accretion data and simulations of radioactive heating effects.

Findings

White dwarfs often accrete iron-rich planetary material.

Radioactive nuclides like Al-2 likely caused heating for core formation.

Planetesimal formation occurs within a few hundred thousand years after cloud collapse.

Abstract

The timing of formation for the first planetesimals determines the mode of planetary accretion and their geophysical and compositional evolution. Astronomical observations of circumstellar discs and Solar System geochronology provide evidence for planetesimal formation during molecular cloud collapse, much earlier than previously estimated. Here, we present distinct observational evidence from white dwarf planetary systems for planetesimal formation occurring during the first few hundred thousand years after cloud collapse in exoplanetary systems. A significant fraction of white dwarfs have accreted planetary material rich in iron core or mantle material. In order for the exo-asteroids accreted by white dwarfs to form iron cores, substantial heating is required. By simulating planetesimal evolution and collisional evolution we show that the most likely heat source is short-lived radioactive nuclides such as Al-2 (half life of approximately 0.7 Myr). Core-rich materials in the atmospheres of white dwarfs, therefore, provide independent evidence for rapid planetesimal formation, concurrent with star formation.