The properties of supermassive stars in galaxy merger driven direct collapse I: models without rotation
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arXiv
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| Format: | Preprint |
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2025
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| _version_ | 1866912520322678784 |
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| author | Haemmerlé, Lionel |
| author_facet | Haemmerlé, Lionel |
| contents | The formation of the most massive quasars observed at high redshifts requires extreme accretion rates ($>1$ M$_\odot$ yr$^{-1}$). Inflows of $10-1000$ M$_\odot$ yr$^{-1}$ are found in hydrodynamical simulations of galaxy mergers, leading to the formation of supermassive discs (SMDs) with high metallicities ($>$ Z$_\odot$). Supermassive stars (SMSs) born in these SMDs could be the progenitors of the most extreme quasars. Here, we study the properties of non-rotating SMSs forming in high metallicity SMDs. Using the stellar evolution code GENEC, we compute numerically the hydrostatic structures of non-rotating SMSs with metallicities $Z=1-10$ Z$_\odot$ by following their evolution under constant accretion at rates $10-1000$ M$_\odot$ yr$^{-1}$. We determine the final mass of the SMSs, set by the general-relativistic (GR) instability, by applying the relativistic equation of adiabatic pulsations to the hydrostatic structures. We find that non-rotating SMSs with metallicities $Z=1-10$ Z$_\odot$ accreting at rates $10-1000$ M$_\odot$ yr$^{-1}$ evolve as red supergiant protostars until their final collapse. All the models reach the GR instability during H-burning. The final mass is $\sim10^6$ M$_\odot$, nearly independently of the metallicity and the accretion rate. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_01970 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The properties of supermassive stars in galaxy merger driven direct collapse I: models without rotation Haemmerlé, Lionel High Energy Astrophysical Phenomena Astrophysics of Galaxies Solar and Stellar Astrophysics The formation of the most massive quasars observed at high redshifts requires extreme accretion rates ($>1$ M$_\odot$ yr$^{-1}$). Inflows of $10-1000$ M$_\odot$ yr$^{-1}$ are found in hydrodynamical simulations of galaxy mergers, leading to the formation of supermassive discs (SMDs) with high metallicities ($>$ Z$_\odot$). Supermassive stars (SMSs) born in these SMDs could be the progenitors of the most extreme quasars. Here, we study the properties of non-rotating SMSs forming in high metallicity SMDs. Using the stellar evolution code GENEC, we compute numerically the hydrostatic structures of non-rotating SMSs with metallicities $Z=1-10$ Z$_\odot$ by following their evolution under constant accretion at rates $10-1000$ M$_\odot$ yr$^{-1}$. We determine the final mass of the SMSs, set by the general-relativistic (GR) instability, by applying the relativistic equation of adiabatic pulsations to the hydrostatic structures. We find that non-rotating SMSs with metallicities $Z=1-10$ Z$_\odot$ accreting at rates $10-1000$ M$_\odot$ yr$^{-1}$ evolve as red supergiant protostars until their final collapse. All the models reach the GR instability during H-burning. The final mass is $\sim10^6$ M$_\odot$, nearly independently of the metallicity and the accretion rate. |
| title | The properties of supermassive stars in galaxy merger driven direct collapse I: models without rotation |
| topic | High Energy Astrophysical Phenomena Astrophysics of Galaxies Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2503.01970 |