A super-Chandrasekhar mass type Ia supernova progenitor at 49 pc set to detonate in 23 Gyr
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| Autores principales: | , , , , , , , , , , , |
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| Formato: | Preprint |
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2025
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| author | Munday, James Pakmor, Ruediger Pelisoli, Ingrid Jones, David Sahu, Snehalata Tremblay, Pier-Emmanuel Rajamuthukumar, Abinaya Swaruba Nelemans, Gijs Magee, Mark Toonen, Silvia Bédard, Antoine Cunningham, Tim |
| author_facet | Munday, James Pakmor, Ruediger Pelisoli, Ingrid Jones, David Sahu, Snehalata Tremblay, Pier-Emmanuel Rajamuthukumar, Abinaya Swaruba Nelemans, Gijs Magee, Mark Toonen, Silvia Bédard, Antoine Cunningham, Tim |
| contents | Double white dwarf binaries are a leading explanation to the origin of type Ia supernovae, but no system exceeding the Chandrasekhar mass limit (1.4 M$_\odot$) has been found that will explode anywhere close to a Hubble time. Here, we present the super-Chandrasekhar mass double white dwarf WDJ181058.67+311940.94 whose merger time ($22.6\pm1.0$ Gyr) is of the same order as a Hubble time. The mass of the binary is large, combining to $1.555\pm0.044$ M$_\odot$, while being located only 49 pc away. We predict that the binary will explode dynamically via a double detonation destroying both stars just before they merge, appearing as a subluminous type Ia supernova with a peak apparent magnitude of about $m_V=-16$ (200,000 times brighter than Jupiter). The observationally-derived birthrate of super-Chandrasekhar mass double white dwarfs is now at least $6.0\times10^{-4}$ yr$^{-1}$ and the observed rate of type Ia supernovae in the Milky Way from such systems is approximately $4.4\times10^{-5}$ yr$^{-1}$, while the predicted type Ia supernova rate in the Milky Way from all progenitor channels is about sixty times larger. Hence, WDJ181058.67+311940.94 mitigates the observed deficit of massive double white dwarfs witnessed in volume-complete populations, but further evidence is required to determine the majority progenitors of type Ia supernovae. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_04522 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A super-Chandrasekhar mass type Ia supernova progenitor at 49 pc set to detonate in 23 Gyr Munday, James Pakmor, Ruediger Pelisoli, Ingrid Jones, David Sahu, Snehalata Tremblay, Pier-Emmanuel Rajamuthukumar, Abinaya Swaruba Nelemans, Gijs Magee, Mark Toonen, Silvia Bédard, Antoine Cunningham, Tim Solar and Stellar Astrophysics High Energy Astrophysical Phenomena Double white dwarf binaries are a leading explanation to the origin of type Ia supernovae, but no system exceeding the Chandrasekhar mass limit (1.4 M$_\odot$) has been found that will explode anywhere close to a Hubble time. Here, we present the super-Chandrasekhar mass double white dwarf WDJ181058.67+311940.94 whose merger time ($22.6\pm1.0$ Gyr) is of the same order as a Hubble time. The mass of the binary is large, combining to $1.555\pm0.044$ M$_\odot$, while being located only 49 pc away. We predict that the binary will explode dynamically via a double detonation destroying both stars just before they merge, appearing as a subluminous type Ia supernova with a peak apparent magnitude of about $m_V=-16$ (200,000 times brighter than Jupiter). The observationally-derived birthrate of super-Chandrasekhar mass double white dwarfs is now at least $6.0\times10^{-4}$ yr$^{-1}$ and the observed rate of type Ia supernovae in the Milky Way from such systems is approximately $4.4\times10^{-5}$ yr$^{-1}$, while the predicted type Ia supernova rate in the Milky Way from all progenitor channels is about sixty times larger. Hence, WDJ181058.67+311940.94 mitigates the observed deficit of massive double white dwarfs witnessed in volume-complete populations, but further evidence is required to determine the majority progenitors of type Ia supernovae. |
| title | A super-Chandrasekhar mass type Ia supernova progenitor at 49 pc set to detonate in 23 Gyr |
| topic | Solar and Stellar Astrophysics High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2504.04522 |