The coolest extremely low-mass white dwarfs

• Autores: Calcaferro, Leila Magdalena; Althaus, Leandro Gabriel; Córsico, Alejandro Hugo
• Año de publicación: 2018
• Idioma: inglés
• Tipo de recurso: artículo
• Materia: Astronomía; stars: evolution; stars: interiors; stars: individual: ELM WD; white dwarfs
• Institución: Universidad Nacional de La Plata

Context. Extremely low-mass white dwarf (ELM WD; M⁎ ≲ 0.18-0.20 M⊙) stars are thought to be formed in binary systems via stable or unstable mass transfer. Although stable mass transfer predicts the formation of ELM WDs with thick hydrogen (H) envelopes that are characterized by dominant residual nuclear burning along the cooling branch, the formation of ELM WDs with thinner H envelopes from unstable mass loss cannot be discarded. Aims. We compute new evolutionary sequences for helium (He) core WD stars with thin H envelopes with the main aim of assessing the lowest T_eff that could be reached by this type of stars. Methods. We generate a new grid of evolutionary sequences of He-core WD stars with thin H envelopes in the mass range from 0.1554 to 0.2025 M⊙, and assess the changes in both the cooling times and surface gravity induced by a reduction of the H envelope. We also determine, taking into account the predictions of progenitor evolution, the lowest T_eff reached by the resulting ELM WDs. Results. We find that a slight reduction in the H envelope yields a significant increase in the cooling rate of ELM WDs. Because of this, ELM WDs with thin H envelopes could cool down to ∼2500 K, in contrast to their canonical counterparts that cool down to ∼7000 K. In addition, we find that a reduction of the thickness of the H envelope markedly increases the surface gravity (g) of these stars. Conclusions. If ELM WDs are formed with thin H envelopes, they could be detected at very low T_eff. The detection of such cool ELM WDs would be indicative that they were formed with thin H envelopes, thus opening the possibility of placing constraints on the possible mechanisms of formation of this type of star. Last but not least, the increase in g due to the reduction of the H envelope leads to consequences in the spectroscopic determinations of these stars.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata