Effect of mass-loss due to stellar winds on the formation of supermassive black hole seeds in dense nuclear star clusters
The observations of high-redshifts quasars at z ≳ 6 have revealed that supermassive black holes (SMBHs) of mass ∼109M⊙∼109M⊙ were already in place within the first ∼Gyr after the big bang. Supermassive stars (SMSs) with masses 103−5M⊙103−5M⊙ are potential seeds for these observed SMBHs. A possible f...
| Main Authors: | , , , |
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| Format: | Journal article |
| Language: | English |
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Oxford University Press
2021
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| _version_ | 1826292595094978560 |
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| author | Das, A Schleicher, DRG Basu, S Boekholt, TCN |
| author_facet | Das, A Schleicher, DRG Basu, S Boekholt, TCN |
| author_sort | Das, A |
| collection | OXFORD |
| description | The observations of high-redshifts quasars at z ≳ 6 have revealed that supermassive black holes (SMBHs) of mass ∼109M⊙∼109M⊙ were already in place within the first ∼Gyr after the big bang. Supermassive stars (SMSs) with masses 103−5M⊙103−5M⊙ are potential seeds for these observed SMBHs. A possible formation channel of these SMSs is the interplay of gas accretion and runaway stellar collisions inside dense nuclear star clusters (NSCs). However, mass-loss due to stellar winds could be an important limitation for the formation of the SMSs and affect the final mass. In this paper, we study the effect of mass-loss driven by stellar winds on the formation and evolution of SMSs in dense NSCs using idealized N-body simulations. Considering different accretion scenarios, we have studied the effect of the mass-loss rates over a wide range of metallicities Z* = [.001–1]Z⊙ and Eddington factors fEdd=L∗/LEdd=0.5,0.7,and0.9fEdd=L∗/LEdd=0.5,0.7,and0.9. For a high accretion rate of 10−4M⊙yr−110−4M⊙yr−1, SMSs with masses ≳103M⊙yr−1≳103M⊙yr−1 could be formed even in a high metallicity environment. For a lower accretion rate of 10−5M⊙yr−110−5M⊙yr−1, SMSs of masses ∼103−4M⊙∼103−4M⊙ can be formed for all adopted values of Z* and fEdd, except for Z* = Z⊙ and fEdd = 0.7 or 0.9. For Eddington accretion, SMSs of masses ∼103M⊙∼103M⊙ can be formed in low metallicity environments with Z* ≲ 0.01 Z⊙. The most massive SMSs of masses ∼105M⊙∼105M⊙ can be formed for Bondi–Hoyle accretion in environments with Z* ≲ 0.5 Z⊙. An intermediate regime is likely to exist where the mass-loss from the winds might no longer be relevant, while the kinetic energy deposition from the wind could still inhibit the formation of a very massive object. |
| first_indexed | 2024-03-07T03:17:07Z |
| format | Journal article |
| id | oxford-uuid:b62bb4f7-0912-4f40-8b9c-f4fb55889019 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-07T03:17:07Z |
| publishDate | 2021 |
| publisher | Oxford University Press |
| record_format | dspace |
| spelling | oxford-uuid:b62bb4f7-0912-4f40-8b9c-f4fb558890192022-03-27T04:39:00ZEffect of mass-loss due to stellar winds on the formation of supermassive black hole seeds in dense nuclear star clustersJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:b62bb4f7-0912-4f40-8b9c-f4fb55889019EnglishSymplectic ElementsOxford University Press2021Das, ASchleicher, DRGBasu, SBoekholt, TCNThe observations of high-redshifts quasars at z ≳ 6 have revealed that supermassive black holes (SMBHs) of mass ∼109M⊙∼109M⊙ were already in place within the first ∼Gyr after the big bang. Supermassive stars (SMSs) with masses 103−5M⊙103−5M⊙ are potential seeds for these observed SMBHs. A possible formation channel of these SMSs is the interplay of gas accretion and runaway stellar collisions inside dense nuclear star clusters (NSCs). However, mass-loss due to stellar winds could be an important limitation for the formation of the SMSs and affect the final mass. In this paper, we study the effect of mass-loss driven by stellar winds on the formation and evolution of SMSs in dense NSCs using idealized N-body simulations. Considering different accretion scenarios, we have studied the effect of the mass-loss rates over a wide range of metallicities Z* = [.001–1]Z⊙ and Eddington factors fEdd=L∗/LEdd=0.5,0.7,and0.9fEdd=L∗/LEdd=0.5,0.7,and0.9. For a high accretion rate of 10−4M⊙yr−110−4M⊙yr−1, SMSs with masses ≳103M⊙yr−1≳103M⊙yr−1 could be formed even in a high metallicity environment. For a lower accretion rate of 10−5M⊙yr−110−5M⊙yr−1, SMSs of masses ∼103−4M⊙∼103−4M⊙ can be formed for all adopted values of Z* and fEdd, except for Z* = Z⊙ and fEdd = 0.7 or 0.9. For Eddington accretion, SMSs of masses ∼103M⊙∼103M⊙ can be formed in low metallicity environments with Z* ≲ 0.01 Z⊙. The most massive SMSs of masses ∼105M⊙∼105M⊙ can be formed for Bondi–Hoyle accretion in environments with Z* ≲ 0.5 Z⊙. An intermediate regime is likely to exist where the mass-loss from the winds might no longer be relevant, while the kinetic energy deposition from the wind could still inhibit the formation of a very massive object. |
| spellingShingle | Das, A Schleicher, DRG Basu, S Boekholt, TCN Effect of mass-loss due to stellar winds on the formation of supermassive black hole seeds in dense nuclear star clusters |
| title | Effect of mass-loss due to stellar winds on the formation of supermassive black hole seeds in dense nuclear star clusters |
| title_full | Effect of mass-loss due to stellar winds on the formation of supermassive black hole seeds in dense nuclear star clusters |
| title_fullStr | Effect of mass-loss due to stellar winds on the formation of supermassive black hole seeds in dense nuclear star clusters |
| title_full_unstemmed | Effect of mass-loss due to stellar winds on the formation of supermassive black hole seeds in dense nuclear star clusters |
| title_short | Effect of mass-loss due to stellar winds on the formation of supermassive black hole seeds in dense nuclear star clusters |
| title_sort | effect of mass loss due to stellar winds on the formation of supermassive black hole seeds in dense nuclear star clusters |
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