Pulsating low-mass white dwarfs in the frame of new evolutionary sequences: V. Asteroseismology of ELMV white dwarf stars

TL;DR

This study uses detailed evolutionary models to perform asteroseismology on known low-mass white dwarf stars, constraining their internal structure and properties through pulsation period analysis.

Contribution

It provides a comprehensive asteroseismological analysis of low-mass white dwarfs using new evolutionary sequences and compares observed periods with theoretical models to estimate stellar parameters.

Findings

Seismological models generally agree with spectroscopic data for most stars.

Period spacing analysis can estimate stellar mass, but has limitations with few observed periods.

Discrepancies in mass estimates highlight the need for improved models and more observations.

Abstract

Many pulsating low-mass white-dwarf stars have been detected in the last years in the field of our Galaxy. Given that some of them exhibit multiperiodic variation of brightness, it is possible to probe their interiors through asteroseismology. We present a detailed asteroseismological study of all the known low-mass variable white dwarf stars based on a complete set of fully evolutionary models representative of low-mass He-core white dwarf stars. We employed adiabatic radial and nonradial pulsation periods for low-mass white dwarf models with stellar masses ranging from $0.1554$ to $0.4352\ M_{\odot}$, that were derived by simulating the nonconservative evolution of a binary system consisting of an initially $1 M_{\odot}$ ZAMS star and a $1.4 M_{\odot}$ neutron star companion. We estimated the mean period spacing for the stars under study and then we used the comparison between the observed period spacing with the average of the computed period spacings for our grid of models to constrain the stellar mass. We also employed the individual observed periods of every known pulsating low-mass white dwarf star, to search for a representative seismological model. We found that even though the stars under analysis exhibit few periods and the period fits show multiplicity of solutions, it is possible to find seismological models whose mass and effective temperature are in agreement with the values given by spectroscopy, for most of the cases. In the two cases where we could extract the period spacing from the set of observed periods, this method led to values of the stellar masses substantially larger than expected for this type of stars. The results presented in this work show in the one hand, the need for further photometric searches, and on the other hand, some improvements of the theoretical models, in order to place the asteroseismological results on a firmer ground.