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| Main Authors: | , , , , , , , , |
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| Formato: | Preprint |
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2024
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| Acceso en liña: | https://arxiv.org/abs/2402.04443 |
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| author | Rebassa-Mansergas, Alberto Hollands, Mark Parsons, Steven G. Althaus, Leandro G. Pelisoli, Ingrid Irawati, Puji Raddi, Roberto Camisassa, Maria E. Torres, Santiago |
| author_facet | Rebassa-Mansergas, Alberto Hollands, Mark Parsons, Steven G. Althaus, Leandro G. Pelisoli, Ingrid Irawati, Puji Raddi, Roberto Camisassa, Maria E. Torres, Santiago |
| contents | Ultra-short period compact binaries are important sources of gravitational waves, which include e.g. the progenitors of type Ia supernovae or the progenitors of merger episodes that may lead to massive and magnetic single white dwarfs. J0526+5934 is an unresolved compact binary star with an orbital period of 20.5 minutes that belongs to this category. The visible component of J0526+5934 has been recently claimed to be a hot sub-dwarf star with a CO white dwarf companion. Our aim is to provide strong observational plus theoretical evidence that the primary star is rather an extremely-low mass white dwarf, although the hot subdwarf nature cannot be completely ruled out. We analyse optical spectra together with time-series photometry of the visible component of J0526+5934 to constrain its orbital and stellar parameters. We also employ evolutionary sequences for low-mass white dwarfs to derive independent values of the primary mass. From the analysis of our observational data, we find a stellar mass for the primary star in J0526+5934 of 0.26+-0.05 Msun, which perfectly matches the 0.237+-0.035 Msun independent measurement we derived from the theoretical evolutionary models. This value is considerably lower than the theoretically expected and generally observed mass range of hot subdwarf stars, but falls well within the mass limit values of extremely low-mass white dwarfs. We conclude J0526+5934 is the fifth ultra-short period detached double white dwarf currently known. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2402_04443 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | J0526+5934: a peculiar ultra-short period double white dwarf Rebassa-Mansergas, Alberto Hollands, Mark Parsons, Steven G. Althaus, Leandro G. Pelisoli, Ingrid Irawati, Puji Raddi, Roberto Camisassa, Maria E. Torres, Santiago Solar and Stellar Astrophysics High Energy Astrophysical Phenomena Ultra-short period compact binaries are important sources of gravitational waves, which include e.g. the progenitors of type Ia supernovae or the progenitors of merger episodes that may lead to massive and magnetic single white dwarfs. J0526+5934 is an unresolved compact binary star with an orbital period of 20.5 minutes that belongs to this category. The visible component of J0526+5934 has been recently claimed to be a hot sub-dwarf star with a CO white dwarf companion. Our aim is to provide strong observational plus theoretical evidence that the primary star is rather an extremely-low mass white dwarf, although the hot subdwarf nature cannot be completely ruled out. We analyse optical spectra together with time-series photometry of the visible component of J0526+5934 to constrain its orbital and stellar parameters. We also employ evolutionary sequences for low-mass white dwarfs to derive independent values of the primary mass. From the analysis of our observational data, we find a stellar mass for the primary star in J0526+5934 of 0.26+-0.05 Msun, which perfectly matches the 0.237+-0.035 Msun independent measurement we derived from the theoretical evolutionary models. This value is considerably lower than the theoretically expected and generally observed mass range of hot subdwarf stars, but falls well within the mass limit values of extremely low-mass white dwarfs. We conclude J0526+5934 is the fifth ultra-short period detached double white dwarf currently known. |
| title | J0526+5934: a peculiar ultra-short period double white dwarf |
| topic | Solar and Stellar Astrophysics High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2402.04443 |