Formation of Massive and Wide First-star Binaries in Radiation Hydrodynamic Simulations
We study the formation of Population III stars by performing radiation hydrodynamic simulations for three different initial clouds extracted from cosmological hydrodynamic simulations. Starting from the cloud collapse stage, we follow the growth of protostars by accretion for ∼10 ^5 yr until the rad...
| Main Authors: | , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad02fc |
| _version_ | 1827630011984642048 |
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| author | Kazuyuki Sugimura Tomoaki Matsumoto Takashi Hosokawa Shingo Hirano Kazuyuki Omukai |
| author_facet | Kazuyuki Sugimura Tomoaki Matsumoto Takashi Hosokawa Shingo Hirano Kazuyuki Omukai |
| author_sort | Kazuyuki Sugimura |
| collection | DOAJ |
| description | We study the formation of Population III stars by performing radiation hydrodynamic simulations for three different initial clouds extracted from cosmological hydrodynamic simulations. Starting from the cloud collapse stage, we follow the growth of protostars by accretion for ∼10 ^5 yr until the radiative feedback from the protostars suppresses the accretion and the stellar properties are nearly fixed. We find that Population III stars form in massive and wide binary/small-multiple stellar systems, with masses >30 M _⊙ and separations >2000 au. We also find that the properties of the final stellar system correlate with those of the initial clouds: the total mass increases with the cloud-scale accretion rate, and the angular momentum of the binary orbit matches that of the initial cloud. While the total mass of the system in our simulations is consistent with our previous single-star formation simulations, individual masses are lower due to mass sharing, suggesting potential modification in the extent of feedback from Population III stars in the subsequent evolution of the Universe. We also identify such systems as mini-binaries embedded in a wider outer multiple-star system, which could evolve into progenitors for observed gravitational wave events. |
| first_indexed | 2024-03-09T14:00:22Z |
| format | Article |
| id | doaj.art-d0f63849e57d4148af80a2b0d6326cee |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-09T14:00:22Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-d0f63849e57d4148af80a2b0d6326cee2023-11-30T09:31:29ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0195911710.3847/1538-4357/ad02fcFormation of Massive and Wide First-star Binaries in Radiation Hydrodynamic SimulationsKazuyuki Sugimura0https://orcid.org/0000-0001-7842-5488Tomoaki Matsumoto1https://orcid.org/0000-0002-8125-4509Takashi Hosokawa2https://orcid.org/0000-0003-3127-5982Shingo Hirano3https://orcid.org/0000-0002-4317-767XKazuyuki Omukai4https://orcid.org/0000-0001-5922-180XFaculty of Science, Hokkaido University , Sapporo, Hokkaido 060-0810, Japan ; sugimura@sci.hokudai.ac.jp; The Hakubi Center for Advanced Research, Kyoto University , Sakyo, Kyoto 606-8501, Japan; Department of Physics, Kyoto University , Sakyo, Kyoto 606-8502, JapanFaculty of Sustainability Studies, Hosei University , Fujimi, Chiyoda, Tokyo 102-8160, JapanDepartment of Physics, Kyoto University , Sakyo, Kyoto 606-8502, JapanDepartment of Astronomy, School of Science, University of Tokyo , Tokyo 113-0033, JapanAstronomical Institute, Graduate School of Science, Tohoku University , Aoba, Sendai 980-8578, JapanWe study the formation of Population III stars by performing radiation hydrodynamic simulations for three different initial clouds extracted from cosmological hydrodynamic simulations. Starting from the cloud collapse stage, we follow the growth of protostars by accretion for ∼10 ^5 yr until the radiative feedback from the protostars suppresses the accretion and the stellar properties are nearly fixed. We find that Population III stars form in massive and wide binary/small-multiple stellar systems, with masses >30 M _⊙ and separations >2000 au. We also find that the properties of the final stellar system correlate with those of the initial clouds: the total mass increases with the cloud-scale accretion rate, and the angular momentum of the binary orbit matches that of the initial cloud. While the total mass of the system in our simulations is consistent with our previous single-star formation simulations, individual masses are lower due to mass sharing, suggesting potential modification in the extent of feedback from Population III stars in the subsequent evolution of the Universe. We also identify such systems as mini-binaries embedded in a wider outer multiple-star system, which could evolve into progenitors for observed gravitational wave events.https://doi.org/10.3847/1538-4357/ad02fcPopulation III starsEarly universeStar formation |
| spellingShingle | Kazuyuki Sugimura Tomoaki Matsumoto Takashi Hosokawa Shingo Hirano Kazuyuki Omukai Formation of Massive and Wide First-star Binaries in Radiation Hydrodynamic Simulations The Astrophysical Journal Population III stars Early universe Star formation |
| title | Formation of Massive and Wide First-star Binaries in Radiation Hydrodynamic Simulations |
| title_full | Formation of Massive and Wide First-star Binaries in Radiation Hydrodynamic Simulations |
| title_fullStr | Formation of Massive and Wide First-star Binaries in Radiation Hydrodynamic Simulations |
| title_full_unstemmed | Formation of Massive and Wide First-star Binaries in Radiation Hydrodynamic Simulations |
| title_short | Formation of Massive and Wide First-star Binaries in Radiation Hydrodynamic Simulations |
| title_sort | formation of massive and wide first star binaries in radiation hydrodynamic simulations |
| topic | Population III stars Early universe Star formation |
| url | https://doi.org/10.3847/1538-4357/ad02fc |
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