Two unseen massive white dwarf candidates in close binaries
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arXiv
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| Autores principales: | , , , , , , , , , , , , |
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| Formato: | Preprint |
| Publicado: |
2025
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| _version_ | 1866912905332523008 |
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| author | Shiraishi, Yuta Hotokezaka, Kenta Masuda, Kento Honda, Satoshi Tanikawa, Ataru Janssens, Soetkin Tokuno, Takato Shimasue, Takumi Honjo, Ryoga Sato, Bun'ei Omiya, Masashi Tajitsu, Akito Izumiura, Hideyuki |
| author_facet | Shiraishi, Yuta Hotokezaka, Kenta Masuda, Kento Honda, Satoshi Tanikawa, Ataru Janssens, Soetkin Tokuno, Takato Shimasue, Takumi Honjo, Ryoga Sato, Bun'ei Omiya, Masashi Tajitsu, Akito Izumiura, Hideyuki |
| contents | We report the discovery of two binary systems, each consisting of a slightly bloated G-type main-sequence star and an unseen companion, identified through photometric data from TESS and radial velocity variation from Gaia. High-resolution spectroscopy confirms orbital periods of 1.37 and 2 .67 d with circular orbits. The visible components have masses of $\sim$0.9--1.0$\,M_\odot$, while the minimum masses of the unseen companions are $1.078^{+0.058}_{-0.060}\, M_\odot$ and $0.943^{+0.048}_{-0.049}\, M_\odot$, respectively. Assuming tidal synchronization, we estimate the companion masses to be $1.13^{+0.11}_{-0.08} M_\odot$ and $1.05^{+0.15}_{-0.10} M_\odot$. The absence of detectable spectral features from the companions rules out main-sequence stars of these masses, suggesting that the unseen companions are likely O/Ne or C/O massive white dwarfs. The short orbital periods imply that these systems are post-common envelope binaries. Their subsequent evolution is uncertain, with possible outcomes including cataclysmic variables, Type Ia supernovae, or accretion-induced collapse, depending on the nature of future mass transfer. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2509_12808 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Two unseen massive white dwarf candidates in close binaries Shiraishi, Yuta Hotokezaka, Kenta Masuda, Kento Honda, Satoshi Tanikawa, Ataru Janssens, Soetkin Tokuno, Takato Shimasue, Takumi Honjo, Ryoga Sato, Bun'ei Omiya, Masashi Tajitsu, Akito Izumiura, Hideyuki Solar and Stellar Astrophysics We report the discovery of two binary systems, each consisting of a slightly bloated G-type main-sequence star and an unseen companion, identified through photometric data from TESS and radial velocity variation from Gaia. High-resolution spectroscopy confirms orbital periods of 1.37 and 2 .67 d with circular orbits. The visible components have masses of $\sim$0.9--1.0$\,M_\odot$, while the minimum masses of the unseen companions are $1.078^{+0.058}_{-0.060}\, M_\odot$ and $0.943^{+0.048}_{-0.049}\, M_\odot$, respectively. Assuming tidal synchronization, we estimate the companion masses to be $1.13^{+0.11}_{-0.08} M_\odot$ and $1.05^{+0.15}_{-0.10} M_\odot$. The absence of detectable spectral features from the companions rules out main-sequence stars of these masses, suggesting that the unseen companions are likely O/Ne or C/O massive white dwarfs. The short orbital periods imply that these systems are post-common envelope binaries. Their subsequent evolution is uncertain, with possible outcomes including cataclysmic variables, Type Ia supernovae, or accretion-induced collapse, depending on the nature of future mass transfer. |
| title | Two unseen massive white dwarf candidates in close binaries |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2509.12808 |