{"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_created":"2024-09-05T12:33:59Z","author":[{"last_name":"Toyouchi","first_name":"Daisuke","full_name":"Toyouchi, Daisuke"},{"last_name":"Inayoshi","full_name":"Inayoshi, Kohei","first_name":"Kohei"},{"last_name":"Li","full_name":"Li, Wenxiu","first_name":"Wenxiu"},{"last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","full_name":"Haiman, Zoltán"},{"last_name":"Kuiper","full_name":"Kuiper, Rolf","first_name":"Rolf"}],"page":"1601-1616","issue":"2","language":[{"iso":"eng"}],"date_published":"2022-11-09T00:00:00Z","article_type":"original","main_file_link":[{"url":"https://doi.org/10.1093/mnras/stac3191","open_access":"1"}],"status":"public","day":"09","date_updated":"2024-09-19T12:06:18Z","oa_version":"Published Version","citation":{"ista":"Toyouchi D, Inayoshi K, Li W, Haiman Z, Kuiper R. 2022. Radiative feedback on supermassive star formation: the massive end of the population III initial mass function. Monthly Notices of the Royal Astronomical Society. 518(2), 1601–1616.","ieee":"D. Toyouchi, K. Inayoshi, W. Li, Z. Haiman, and R. Kuiper, “Radiative feedback on supermassive star formation: the massive end of the population III initial mass function,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 518, no. 2. Oxford University Press, pp. 1601–1616, 2022.","ama":"Toyouchi D, Inayoshi K, Li W, Haiman Z, Kuiper R. Radiative feedback on supermassive star formation: the massive end of the population III initial mass function. <i>Monthly Notices of the Royal Astronomical Society</i>. 2022;518(2):1601-1616. doi:<a href=\"https://doi.org/10.1093/mnras/stac3191\">10.1093/mnras/stac3191</a>","short":"D. Toyouchi, K. Inayoshi, W. Li, Z. Haiman, R. Kuiper, Monthly Notices of the Royal Astronomical Society 518 (2022) 1601–1616.","chicago":"Toyouchi, Daisuke, Kohei Inayoshi, Wenxiu Li, Zoltán Haiman, and Rolf Kuiper. “Radiative Feedback on Supermassive Star Formation: The Massive End of the Population III Initial Mass Function.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2022. <a href=\"https://doi.org/10.1093/mnras/stac3191\">https://doi.org/10.1093/mnras/stac3191</a>.","apa":"Toyouchi, D., Inayoshi, K., Li, W., Haiman, Z., &#38; Kuiper, R. (2022). Radiative feedback on supermassive star formation: the massive end of the population III initial mass function. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stac3191\">https://doi.org/10.1093/mnras/stac3191</a>","mla":"Toyouchi, Daisuke, et al. “Radiative Feedback on Supermassive Star Formation: The Massive End of the Population III Initial Mass Function.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 518, no. 2, Oxford University Press, 2022, pp. 1601–16, doi:<a href=\"https://doi.org/10.1093/mnras/stac3191\">10.1093/mnras/stac3191</a>."},"type":"journal_article","publisher":"Oxford University Press","oa":1,"doi":"10.1093/mnras/stac3191","publication":"Monthly Notices of the Royal Astronomical Society","year":"2022","publication_identifier":{"issn":["0035-8711","1365-2966"]},"month":"11","scopus_import":"1","quality_controlled":"1","article_processing_charge":"No","intvolume":"       518","abstract":[{"text":"Supermassive stars (SMSs) with masses of M∗≃104--105 M⊙ are invoked as possible seeds of high-redshift supermassive black holes, but it remains under debate whether their protostar indeed acquires sufficient mass via gas accretion overcoming radiative feedback. We investigate protostellar growth in dynamically heated atomic-cooling haloes (ACHs) found in recent cosmological simulations, performing three-dimensional radiation hydrodynamical (RHD) simulations that consider stellar evolution under variable mass accretion. We find that one of the ACHs feeds the central protostar at rates exceeding a critical value, above which the star evolves in a cool bloating phase and hardly produces ionizing photons. Consequently, the stellar mass reaches M∗≳104 M⊙ unimpeded by radiative feedback. In the other ACH, where the mass supply rate is lower, the star spends most of its life as a hot main-sequence star, emitting intense ionizing radiation. Then, the stellar mass growth is terminated around 500 M⊙ by photoevaporation of the circumstellar disk. A series of our RHD simulations provide a formula of the final stellar mass determined either by stellar feedback or their lifetime as a function of the mass supply rate from the parent cloud in the absence of stellar radiation. Combining the results with the statistical properties of SMS-forming clouds in high-redshift quasar progenitor haloes, we construct a top-heavy mass distribution of primordial stars over M∗≃100--105 M⊙, approximately following a power-law spectrum of ∝M−1.3∗ with a steeper decline at M∗≳2×104 M⊙. Their massive BH remnants would be further fed via the dense debris disk, powering \"milli-quasars\" with a bolometric luminosity of Lbol ≳ 1043 erg s−1.","lang":"eng"}],"publication_status":"published","title":"Radiative feedback on supermassive star formation: the massive end of the population III initial mass function","extern":"1","_id":"17588","volume":518}