The formation of ultra-massive carbon-oxygen core white dwarfs and their evolutionary and pulsational properties

Abstract

Context. The existence of ultra-massive white dwarf stars, MWD ≳ 1.05 M⊙, has been reported in several studies. These white dwarfs are relevant for the role they play in type Ia supernova explosions, the occurrence of physical processes in the asymptotic giant-branch phase, the existence of high-field magnetic white dwarfs, and the occurrence of double-white-dwarf mergers. Aims. We aim to explore the formation of ultra-massive, carbon-oxygen core white dwarfs resulting from single stellar evolution. We also intend to study their evolutionary and pulsational properties and compare them with those of the ultra-massive white dwarfs with oxygen-neon cores resulting from carbon burning in single progenitor stars, and with binary merger predictions. The aim is to provide a theoretical basis that can eventually help to discern the core composition of ultra-massive white dwarfs and the circumstances of their formation. Methods. We considered two single-star evolution scenarios for the formation of ultra-massive carbon-oxygen core white dwarfs, which involve the rotation of the degenerate core after core helium burning and reduced mass-loss rates in massive asymptotic giant-branch stars. We find that reducing standard mass-loss rates by a factor larger than 5−20 yields the formation of carbon-oxygen cores more massive than 1.05 M⊙ as a result of the slow growth of carbon-oxygen core mass during the thermal pulses. We also performed a series of evolutionary tests of solar-metallicity models with initial masses between 4 and 9.5 M⊙ and with different core rotation rates. We find that ultra-massive carbon-oxygen core white dwarfs are formed even for the lowest rotation rates we analyzed, and that the range of initial masses leading to these white dwarfs widens as the rotation rate of the core increases, whereas the initial mass range for the formation of oxygen-neon core white dwarfs decreases significantly. Finally, we compared our findings with the predictions from ultra-massive white dwarfs resulting from the merger of two equal-mass carbon-oxygen core white dwarfs, by assuming complete mixing between them and a carbon-oxygen core for the merged remnant. Results. These two single-evolution scenarios produce ultra-massive white dwarfs with different carbon-oxygen profiles and different helium contents, thus leading to distinctive signatures in the period spectrum and mode-trapping properties of pulsating hydrogen-rich white dwarfs. The resulting ultra-massive carbon-oxygen core white dwarfs evolve markedly slower than their oxygen-neon counterparts. Conclusions. Our study strongly suggests the formation of ultra-massive white dwarfs with carbon-oxygen cores from a single stellar evolution. We find that both the evolutionary and pulsation properties of these white dwarfs are markedly different from those of their oxygen-neon core counterparts and from those white dwarfs with carbon-oxygen cores that might result from double-degenerate mergers. This can eventually be used to discern the core composition of ultra-massive white dwarfs and their formation scenario.

The pulsational properties of ultra-massive DB white dwarfs with carbon-oxygen cores coming from single-star evolution

“…In this paper, we show that pulsational properties of the ultramassive DB WDs are much more strongly dependent on their formation scenario than in the case of the DA WD ones studied in Althaus et al (2021). This is due to the fact that pulsating ultra-massive DB WDs, if they exist, must be much hotter than ultra-massive ZZ Cetis and, therefore, their cores must be less crystallized.…”

“…Given recent studies based on post-merger evolutionary calculations suggesting the formation of an ONe core after a WD merger in ultra-massive WDs (Shen et al 2012;Schwab 2021), the existence of a population of ultra-massive WDs with CO cores (UMCO WDs) is difficult to understand. Recently, Althaus et al (2021) have explored single-evolution scenarios which could lead to the formation of UMCO WDs. These authors have studied the evolutionary and pulsational properties of the resulting DA WDs and compared them with those of ultra-massive WDs with ONe cores, thus establishing a theoretical basis that could eventually help to infer the core composition of ultra-massive WDs and the scenario of their formation.…”

“…These authors have studied the evolutionary and pulsational properties of the resulting DA WDs and compared them with those of ultra-massive WDs with ONe cores, thus establishing a theoretical basis that could eventually help to infer the core composition of ultra-massive WDs and the scenario of their formation. Specifically, Althaus et al (2021) study two possible single evolution scenarios for the formation of UMCO WDs. One scenario exploits wind rates and convective boundary uncertainties during the thermally-pulsing AGB (TP-AGB) phase, and it involves the reduction of these rates below the values given by standard prescriptions (see, e.g., Decin et al 2019).…”

“…The other scenario requires the occurrence of rotation in degenerate CO cores, which is naturally expected as a consequence of core contraction at the end of core helium (He) exhaustion (Dominguez et al 1996). Althaus et al (2021) show that both the evolutionary and pulsational properties of the UMCO WDs that formed through these two single evolution scenarios are markedly different from those of ultra-massive WDs with ONe cores (UMONe WDs). Such differences in evolutionary and pulsational properties may eventually be used to shed light on the core composition of ultra-massive WDs.…”

“…In this paper we extend the scope of the study of Althaus et al (2021) by exploring the pulsational properties of the ultramassive WDs with He-rich atmospheres (DB WDs) resulting from single-star evolution. In the case of H-deficient WDs, the mass distribution shows an apparent deficiency of ultra-massive objects (Tremblay et al 2019a;Kepler et al 2019).…”