AEOS: Star-by-Star Cosmological Simulations of Early Chemical Enrichment and Galaxy Formation
Fuente:
arXiv
Guardado en:
| Autores principales: | , , , , , , , , , |
|---|---|
| Formato: | Preprint |
| Publicado: |
2024
|
| Materias: | |
| Acceso en línea: | |
| Etiquetas: |
Agregar Etiqueta
Sin Etiquetas, Sea el primero en etiquetar este registro!
|
| _version_ | 1866917880744902656 |
|---|---|
| author | Brauer, Kaley Emerick, Andrew Mead, Jennifer Ji, Alexander P. Wise, John H. Bryan, Greg L. Mac Low, Mordecai-Mark Cote, Benoit Andersson, Eric P. Frebel, Anna |
| author_facet | Brauer, Kaley Emerick, Andrew Mead, Jennifer Ji, Alexander P. Wise, John H. Bryan, Greg L. Mac Low, Mordecai-Mark Cote, Benoit Andersson, Eric P. Frebel, Anna |
| contents | The AEOS project introduces a series of high-resolution cosmological simulations that model star-by-star chemical enrichment and galaxy formation in the early Universe, achieving 1 pc resolution. These simulations capture the complexities of galaxy evolution within the first ~300 Myr by modeling individual stars and their feedback processes. By incorporating chemical yields from individual stars, AEOS generates galaxies with diverse stellar chemical abundances, linking them to hierarchical galaxy formation and early nucleosynthetic events. These simulations underscore the importance of chemical abundance patterns in ancient stars as vital probes of early nucleosynthesis, star formation histories, and galaxy formation. We examine the metallicity floors of various elements resulting from Pop III enrichment, providing best-fit values for eight different metals (e.g., [O/H] = -4.0) to guide simulations without Pop III models. Additionally, we identify galaxies that begin star formation with Pop II after external enrichment and investigate the frequency of CEMP stars at varying metallicities. The AEOS simulations offer detailed insights into the relationship between star formation, feedback, and chemical enrichment. Future work will extend these simulations to later epochs to interpret the diverse stellar populations of the Milky Way and its satellites. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2410_16366 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | AEOS: Star-by-Star Cosmological Simulations of Early Chemical Enrichment and Galaxy Formation Brauer, Kaley Emerick, Andrew Mead, Jennifer Ji, Alexander P. Wise, John H. Bryan, Greg L. Mac Low, Mordecai-Mark Cote, Benoit Andersson, Eric P. Frebel, Anna Astrophysics of Galaxies The AEOS project introduces a series of high-resolution cosmological simulations that model star-by-star chemical enrichment and galaxy formation in the early Universe, achieving 1 pc resolution. These simulations capture the complexities of galaxy evolution within the first ~300 Myr by modeling individual stars and their feedback processes. By incorporating chemical yields from individual stars, AEOS generates galaxies with diverse stellar chemical abundances, linking them to hierarchical galaxy formation and early nucleosynthetic events. These simulations underscore the importance of chemical abundance patterns in ancient stars as vital probes of early nucleosynthesis, star formation histories, and galaxy formation. We examine the metallicity floors of various elements resulting from Pop III enrichment, providing best-fit values for eight different metals (e.g., [O/H] = -4.0) to guide simulations without Pop III models. Additionally, we identify galaxies that begin star formation with Pop II after external enrichment and investigate the frequency of CEMP stars at varying metallicities. The AEOS simulations offer detailed insights into the relationship between star formation, feedback, and chemical enrichment. Future work will extend these simulations to later epochs to interpret the diverse stellar populations of the Milky Way and its satellites. |
| title | AEOS: Star-by-Star Cosmological Simulations of Early Chemical Enrichment and Galaxy Formation |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2410.16366 |