The progenitors of magnetic white dwarfs in open clusters

TL;DR

This study investigates the origins of magnetic white dwarfs in open clusters by analyzing their properties, confirming cluster membership, and assessing their progenitor masses to understand the role of magnetism in stellar evolution.

Contribution

It identifies new magnetic white dwarf members in open clusters and evaluates their properties, providing insights into the initial-to-final-mass relation for magnetic white dwarfs.

Findings

Confirmed SDSS J085523.87+164059.0 as a cluster member and ultra-massive white dwarf.

Expanded the sample of magnetic white dwarfs with known progenitor masses to ten.

Found no evidence that magnetism affects the initial-to-final-mass relation when magnetic effects are included.

Abstract

According to the fossil-field hypothesis magnetic fields are remnants of the previous stages of evolution. However, population synthesis calculations are unable to reproduce the magnetic white dwarf (MWD) sample without binary interaction or inclusion of a population of progenitor with unobservable small-scale fields. One necessary ingredient in population synthesis is the initial-to-final-mass relation (IFMR) which describes the mass-loss processes during the stellar evolution. When white dwarfs are members of open clusters, their evolutionary histories can be assessed through the use of cluster properties. In this work, we assess the cluster membership by correlating the proper-motion of MWDs with the cluster proper-motion and by analyzing the candidates spectroscopically with our magnetic model spectra in order to estimate the effective temperature and radii. We identified SDSS J085523.87+164059.0 to be a proper-motion member of Praesepe. We also included the data of the formerly identified cluster members NGC 6819-8, WD 0836+201 and estimated the mass, cooling age and the progenitor masses of the three probable MWD members of open clusters. According to our analysis, the newly identified cluster member SDSS J085523.87+164059.0 is an ultra-massive MWD of mass 1.12 $\pm$ 0.11 Msolar. We increase the sample of MWDs with known progenitor masses to ten, with the rest of the data coming from the common proper motion binaries. Our investigations show that, when effects of the magnetic fields are included in the diagnostics, the estimated properties of these cluster MWDs do not show evidence for deviations from the IFMR. Furthermore, we estimate the precision of the magnetic diagnostics which would be necessary to determine quantitatively whether magnetism has any effect on the mass-loss.