White-dwarf asteroseismology: an update

TL;DR

White-dwarf asteroseismology uses stellar pulsations observed via space missions to probe the internal structure of white dwarfs, advancing understanding of their evolution, composition, and fundamental physics.

Contribution

This paper provides an updated review of white-dwarf asteroseismology, highlighting recent findings from space-mission data and advancements in modeling internal stellar properties.

Findings

Improved constraints on internal chemical stratification.

Enhanced understanding of white dwarf mass and rotation profiles.

Insights into magnetic field strengths in white dwarfs.

Abstract

The vast majority of stars that populate the Universe will end their evolution as white-dwarf stars. Applications of white dwarfs include cosmochronology, evolution of planetary systems, and also as laboratories to study non-standard physics and crystallization. In addition to the knowledge of their surface properties from spectroscopy combined with model atmospheres, the global pulsations that they exhibit during several phases of their evolution allow spying on the deep interior of these stars. Indeed, by means of asteroseismology, an approach based on the comparison between the observed pulsation periods of variable white dwarfs and the periods predicted by representative theoretical models, we can infer details of the internal chemical stratification, the total mass, and even the stellar rotation profile and strength of magnetic fields. In this article, we review the current state of the area, emphasizing the latest findings provided by space-mission data.