{"external_id":{"isi":["001553472000001"],"arxiv":["2501.12986"]},"_id":"20250","issue":"2","article_processing_charge":"Yes","doi":"10.1093/mnras/staf1269","OA_place":"publisher","day":"01","date_created":"2025-08-31T22:01:31Z","type":"journal_article","date_published":"2025-09-01T00:00:00Z","article_type":"original","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"publisher":"Oxford University Press","acknowledgement":"We thank the anonymous referee for comments that helped us improve the clarity of this manuscript. We acknowledge support from the United States National Science Foundation (NSF) grant AST-2006176 and the National Aeronautics and Space Administration (NASA) grants 80NSSC24K0440 and 80NSSC22K0822 (ZH). We also acknowledge support from NSF grant AST-2009309, NASA Astrophysics Theory Program grant 80NSSC22K0629, and Space Telescope Science Institute grant JWST-AR-05238 (EV). The simulations in this work were run on Texas Advanced Computing Center’s Stampede2 and Stampede3 systems. We used Stampede2 and Purdue University’s computing system Anvil for data analysis.","file_date_updated":"2025-09-03T05:44:47Z","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"publication_status":"published","arxiv":1,"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","intvolume":" 542","volume":542,"publication":"Monthly Notices of the Royal Astronomical Society","page":"822-838","file":[{"creator":"dernst","success":1,"access_level":"open_access","file_id":"20279","checksum":"2a06796b27da0b33d479dba170ba4b3f","date_updated":"2025-09-03T05:44:47Z","file_size":2780496,"relation":"main_file","date_created":"2025-09-03T05:44:47Z","file_name":"2025_MonthlyNoticesRAS_Sullivan.pdf","content_type":"application/pdf"}],"isi":1,"citation":{"apa":"Sullivan, J., Haiman, Z., Kulkarni, M., & Visbal, E. (2025). Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback? Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf1269","chicago":"Sullivan, James, Zoltán Haiman, Mihir Kulkarni, and Eli Visbal. “Can Supermassive Stars Form in Protogalaxies Due to Internal Lyman-Werner Feedback?” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf1269.","mla":"Sullivan, James, et al. “Can Supermassive Stars Form in Protogalaxies Due to Internal Lyman-Werner Feedback?” Monthly Notices of the Royal Astronomical Society, vol. 542, no. 2, Oxford University Press, 2025, pp. 822–38, doi:10.1093/mnras/staf1269.","ieee":"J. Sullivan, Z. Haiman, M. Kulkarni, and E. Visbal, “Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback?,” Monthly Notices of the Royal Astronomical Society, vol. 542, no. 2. Oxford University Press, pp. 822–838, 2025.","short":"J. Sullivan, Z. Haiman, M. Kulkarni, E. Visbal, Monthly Notices of the Royal Astronomical Society 542 (2025) 822–838.","ama":"Sullivan J, Haiman Z, Kulkarni M, Visbal E. Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback? Monthly Notices of the Royal Astronomical Society. 2025;542(2):822-838. doi:10.1093/mnras/staf1269","ista":"Sullivan J, Haiman Z, Kulkarni M, Visbal E. 2025. Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback? Monthly Notices of the Royal Astronomical Society. 542(2), 822–838."},"ddc":["520"],"language":[{"iso":"eng"}],"DOAJ_listed":"1","status":"public","scopus_import":"1","has_accepted_license":"1","OA_type":"gold","year":"2025","month":"09","department":[{"_id":"ZoHa"}],"PlanS_conform":"1","title":"Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback?","author":[{"first_name":"James","full_name":"Sullivan, James","last_name":"Sullivan"},{"first_name":"Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","orcid":"0000-0003-3633-5403","full_name":"Haiman, Zoltán"},{"last_name":"Kulkarni","full_name":"Kulkarni, Mihir","first_name":"Mihir"},{"last_name":"Visbal","full_name":"Visbal, Eli","first_name":"Eli"}],"abstract":[{"text":"Population III stars are possible precursors to early supermassive black holes (BHs). The presence of soft UV Lyman–Werner (LW) background radiation can suppress Population III star formation in minihaloes and allow them to form in pristine atomic-cooling haloes. In the absence of molecular hydrogen (H2) cooling, atomic-cooling haloes enable rapid collapse with suppressed fragmentation. High background LW fluxes from preceding star-formation have been proposed to dissociate H2. This flux can be supplemented by LW radiation from one or more Population III star(s) in the same halo, reducing the necessary background level. Here, we consider atomic-cooling haloes in which multiple protostellar cores form close to one another nearly simultaneously. We assess whether the first star’s LW radiation can dissociate nearby \r\n, enabling rapid accretion on to a nearby protostellar core, and the prompt formation of a second, supermassive star (SMS) from warm, atomically-cooled gas. We use a set of hydrodynamical simulations with the code enzo, with identical LW backgrounds centred on a halo with two adjacent collapsing gas clumps. When an additional large local LW flux is introduced, we observe immediate reductions in both the accretion rates and the stellar masses that form within these clumps. While the LW flux reduces the H2 fraction and increases the gas temperature, the halo core’s potential well is too shallow to promptly heat the gas to >1000 K and increase the second protostar’s accretion rate. We conclude that this internal LW feedback scenario is unlikely to facilitate SMS or massive BH seed formation.","lang":"eng"}],"oa_version":"Published Version","quality_controlled":"1","oa":1,"date_updated":"2025-09-30T14:28:05Z"}