How an overweight and rapidly rotating PG 1159 star in the Galactic halo challenges evolutionary models

• Main Authors: Mackensen, Nina, Reindl, Nicole, Werner, Klaus, Dorsch, Matti, Tan, Shuyu
• Format: Journal Article
• Language: English
• Published: 14.07.2025
• Subjects: Physics - Solar and Stellar Astrophysics
• DOI: 10.48550/arxiv.2507.10314

PG 1159 stars are thought to be progenitors of the majority of H-deficient white dwarfs. Their unusual He-, C-, and O-dominated surface composition is typically believed to result from a late thermal pulse experienced by a single (pre-)white dwarf. Yet, other formation channels - involving close binary evolution - have recently been proposed and could lead to similar surface compositions. Here we present a non-local thermodynamic equilibrium spectral analysis based on new UV and archival optical spectra of one of the hottest PG 1159 stars, $\text{RX J}0122.9\text{ -}7521$. We find $T_\text{eff} = 175$ kK and a surface gravity of log $g = 7.7$, and an astonishingly low O/C ratio of $7.3 \times 10^{-3}$ by mass. By combining the spectroscopic surface gravity and Gaia parallax with a spectral energy distribution fit, we derive a mass of $M_\text{spec} = 1.8^{+1.1}_{-0.7}$ $M_\odot$. Although this spectroscopic mass is higher than predicted by evolutionary models, it is subject to substantial uncertainty. Furthermore, we find that $\text{RX J}0122.9\text{ -}7521$ shows strongly rotationally broadened lines, suggesting that the previously reported photometric period of $41$ min indeed corresponds to the rotational period of this star. Our kinematic analysis shows that $\text{RX J}0122.9\text{ -}7521$ belongs to the Galactic halo, which - assuming single-star evolution - is in stark contrast to its relatively high mass. The rapid rotation, high mass, and halo kinematics, as well as the lack of evidence for a close companion, lead us to believe that $\text{RX J}0122.9\text{ -}7521$ formed through the merger of two white dwarfs. Yet, none of the current models can explain the surface abundances of $\text{RX J}0122.9\text{ -}7521$.