Discovery of the Richest Pulsating Ultramassive White Dwarf
The discovery of pulsations in ultramassive (UM) white dwarfs (WDs) can help to probe their interiors and unveil their core composition and crystallized mass fraction through asteroseismic techniques. To date, the richest pulsating UM WD known is BPM 37093 with 8 modes detected, for which detailed a...
| Autores: | , , , , , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2025 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/385346 |
| Acceso en línea: | http://hdl.handle.net/10261/385346 https://api.elsevier.com/content/abstract/scopus_id/85217234264 |
| Access Level: | acceso abierto |
| Palabra clave: | White dwarf stars Stellar oscillations ZZ Ceti stars |
| Sumario: | The discovery of pulsations in ultramassive (UM) white dwarfs (WDs) can help to probe their interiors and unveil their core composition and crystallized mass fraction through asteroseismic techniques. To date, the richest pulsating UM WD known is BPM 37093 with 8 modes detected, for which detailed asteroseismic analysis has been performed in the past. In this work, we report the discovery of 19 pulsation modes in the UM WD star WD J0135+5722, making it the richest pulsating hydrogen-atmosphere UM WD known to date. This object exhibits multiperiodic luminosity variations with periods ranging from 137 to 1345 s, typical of pulsating WDs in the ZZ Ceti instability strip, which is centered at Teff ∼ 12,000 K. We estimate the stellar mass of WD J0135+5722 by different methods, resulting in M⋆ ∼ 1.12-1.14 M⊙ if the star’s core is made of oxygen and neon or M⋆ ∼ 1.14-1.15 M⊙ if the star hosts a carbon oxygen core. Future analysis of the star periods could shed light on the core chemical composition through asteroseismology. |
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