GW231123 Formation from Population III Stars: Isolated Binary Evolution
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arXiv
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| Format: | Preprint |
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2025
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| _version_ | 1866910222871691264 |
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| author | Tanikawa, Ataru Liu, Shuai Wu, WeiWei Fujii, Michiko S. Wang, Long |
| author_facet | Tanikawa, Ataru Liu, Shuai Wu, WeiWei Fujii, Michiko S. Wang, Long |
| contents | GW231123 is a merger of two black holes (BHs) with estimated masses exceeding $100\;{\rm M}_{\odot}$, making them the most massive BHs discovered to date via gravitational wave (GW) observations. We investigate whether GW231123-like events can originate from isolated Population (Pop) III binary stars using binary population synthesis calculations. Our findings indicate that isolated Pop III binaries can produce GW231123-like events at a rate sufficient to explain the discovery of GW231123, provided that three conditions are met: (i) Pop III stars evolve with inefficient convective overshooting, (ii) the $^{12}\text{C}(α, γ)^{16}\text{O}$ rate is $2σ$ lower than the standard value, and (iii) Pop III binary stars share the same orbital parameters as Pop I/II binary stars at the initial time. In contrast, GW190521 -- the most massive BH merger in the Gravitational Wave Transient Catalog 3 -- can be formed from isolated Pop III binaries even with the standard $^{12}\text{C}(α, γ)^{16}\text{O}$ rate. We demonstrate that the discovery of GW231123 is increasingly constraining the parameter ranges of single star evolution models, under the assumption that these GW events originate from isolated binary evolution. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2508_01135 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | GW231123 Formation from Population III Stars: Isolated Binary Evolution Tanikawa, Ataru Liu, Shuai Wu, WeiWei Fujii, Michiko S. Wang, Long Solar and Stellar Astrophysics High Energy Astrophysical Phenomena GW231123 is a merger of two black holes (BHs) with estimated masses exceeding $100\;{\rm M}_{\odot}$, making them the most massive BHs discovered to date via gravitational wave (GW) observations. We investigate whether GW231123-like events can originate from isolated Population (Pop) III binary stars using binary population synthesis calculations. Our findings indicate that isolated Pop III binaries can produce GW231123-like events at a rate sufficient to explain the discovery of GW231123, provided that three conditions are met: (i) Pop III stars evolve with inefficient convective overshooting, (ii) the $^{12}\text{C}(α, γ)^{16}\text{O}$ rate is $2σ$ lower than the standard value, and (iii) Pop III binary stars share the same orbital parameters as Pop I/II binary stars at the initial time. In contrast, GW190521 -- the most massive BH merger in the Gravitational Wave Transient Catalog 3 -- can be formed from isolated Pop III binaries even with the standard $^{12}\text{C}(α, γ)^{16}\text{O}$ rate. We demonstrate that the discovery of GW231123 is increasingly constraining the parameter ranges of single star evolution models, under the assumption that these GW events originate from isolated binary evolution. |
| title | GW231123 Formation from Population III Stars: Isolated Binary Evolution |
| topic | Solar and Stellar Astrophysics High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2508.01135 |