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Very massive stars, pair-instability supernovae and intermediate-mass black holes with the SEVN code

Spera M.
•
Mapelli M.
2017
  • journal article

Periodico
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Abstract
Understanding the link between massive (≳30M⊙) stellar black holes (BHs) and their progenitor stars is a crucial step to interpret observations of gravitational-wave events. In this paper, we discuss the final fate of very massive stars (VMSs), with zero-age main sequence (ZAMS) mass > 150 M⊙, accounting for pulsational pair-instability supernovae (PPISNe) and for pair-instability supernovae (PISNe).We describe an updated version of our population synthesis code SEVN, in which we added stellar evolution tracks for VMSs with ZAMS mass up to 350M⊙ and we included analytical prescriptions for PPISNe and PISNe. We use the new version of SEVN to study the BH mass spectrum at different metallicity Z, ranging from Z = 2.0 × 10-4 to 2.0 × 10-2. The main effect of PPISNe and PISNe is to favour the formation of BHs in the mass range of the first gravitational-wave event (GW150914), while they prevent the formation of remnants with mass 60-120M⊙. In particular, we find that PPISNe significantly enhance mass-loss of metal-poor (Z ≤ 2.0 × 10-3) stars with ZAMS mass 60 = MZAMS/M⊙ ≤ 125. In contrast, PISNe become effective only for moderately metal-poor (Z < 8.0 × 10-3) VMSs. VMSs with mZAMS ≳ 220 M⊙ and Z < 10-3 do not undergo PISNe and form intermediate-mass BHs (with mass ≳200M⊙) via direct collapse.
DOI
10.1093/mnras/stx1576
WOS
WOS:000408207600069
Archivio
http://hdl.handle.net/20.500.11767/122380
info:eu-repo/semantics/altIdentifier/scopus/2-s2.0-85040235053
https://arxiv.org/abs/1706.06109
Diritti
open access
Soggetti
  • Black hole physics

  • Gravitational waves

  • Methods: numerical

  • Stars: massloss

  • Supernovae: general

  • Settore FIS/05 - Astr...

Scopus© citazioni
158
Data di acquisizione
Jun 14, 2022
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Web of Science© citazioni
204
Data di acquisizione
Mar 23, 2024
Visualizzazioni
4
Data di acquisizione
Apr 19, 2024
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