Effect of mass-loss due to stellar winds on the formation of supermassive black hole seeds in dense nuclear star clusters. Issue 2 (19th May 2021)

• Record Type: Journal Article
• Authors: Das, Arpan; Schleicher, Dominik R G; Basu, Shantanu; Boekholt, Tjarda C N
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 505:Issue 2(2021)
• Page Start: 2186
• Page End: 2194
• Publication Date: 2021-05-19
• Subjects: black hole physics -- galaxies: high-redshift; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stab1428
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: The observations of high-redshifts quasars at z ≳ 6 have revealed that supermassive black holes (SMBHs) of mass $\sim 10^9\, \mathrm{M_{\odot }}$ were already in place within the first ∼Gyr after the big bang. Supermassive stars (SMSs) with masses $10^{3-5}\, \mathrm{M_{\odot }}$ 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 $f_{\rm Edd}=L_\ast /L_{\mathrm{Edd}}=0.5, 0.7, \, \, \mathrm{ and}\, 0.9$ . For a high accretion rate of $10^{-4}\, \mathrm{M_{\odot }yr^{-1}}$, SMSs with masses $\gtrsim 10^3\, \mathrm{M_{\odot }yr^{-1}}$ could be formed even in a high metallicity environment. For a lower accretion rate of $10^{-5}\, \mathrm{M_{\odot }yr^{-1}}$, SMSs of masses $\sim 10^{3-4}\, \mathrm{M_{\odot }}$ can be formed for all adopted values of Z * and f Edd, except for Z * = Z⊙ and f Edd = 0.7 or 0.9. For Eddington accretion, SMSs of masses $\sim 10^3\, \mathrm{M_{\odot }}$ can be formed in low metallicity environments with Z * ≲ 0.01 Z⊙ . The most massive SMSs of masses $\sim 10^5\, \mathrm{M_{\odot }}$ 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.