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Dynamics of stellar black holes in young star clusters with different metallicities - I. Implications for X-ray binaries

Mapelli, M.
•
Zampieri, L.
•
Ripamonti, E.
•
Bressan, A.
2013
  • journal article

Periodico
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Abstract
We present N-body simulations of intermediate-mass (3000-4000 M-circle dot) young star clusters (SCs) with three different metallicities (Z = 0.01, 0.1 and 1 Z(circle dot)), including metal-dependent stellar evolution recipes and binary evolution. Following recent theoretical models of wind mass-loss and core-collapse supernovae, we assume that the mass of the stellar remnants depends on the metallicity of the progenitor stars. In particular, massive metal-poor stars (Z = 0.3 Z(circle dot)) are enabled to form massive stellar black holes (MSBHs, with mass >= 25 M-circle dot) through direct collapse. We find that three-body encounters, and especially dynamical exchanges, dominate the evolution of the MSBHs formed in our simulations. In SCs with Z = 0.01 and 0.1 Z(circle dot), about 75 per cent of simulated MSBHs form from single stars and become members of binaries through dynamical exchanges in the first 100 Myr of the SC life. This is a factor of greater than or similar to 3 more efficient than in the case of low-mass (<25 M-circle dot) stellar black holes. A small but non-negligible fraction of MSBHs power wind-accreting (10-20 per cent) and Roche lobe overflow (RLO, 5-10 per cent) binary systems. The vast majority of MSBH binaries that undergo wind accretion and/or RLO were born from dynamical exchange. This result indicates that MSBHs can power X-ray binaries in low-metallicity young SCs, and is very promising to explain the association of many ultraluminous X-ray sources with low-metallicity and actively star-forming environments.
DOI
10.1093/mnras/sts500
WOS
WOS:000318271300032
SCOPUS
2-s2.0-84874047612
Archivio
http://hdl.handle.net/20.500.11767/15987
Diritti
open access
Soggetti
  • black hole physics, m...

  • Settore FIS/05 - Astr...

Web of Science© citazioni
69
Data di acquisizione
May 24, 2022
Scopus© citazioni
74
Data di acquisizione
Jun 2, 2022
Vedi dettagli
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