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

By Mario Spera, Michela Mapelli. 2017

241 citations recorded by the source corpus.

Understanding the link between massive ($\gtrsim 30$ M$_{\odot{}}$) 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$_{\odot}$, 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 $350 $M$_{\odot{}}$ 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 $Z=2.0\times 10^{-4}$ to $Z=2.0\times 10^{-2}$. 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 - 120 M$_{\odot{}}$. In particular, we find that PPISNe significantly enhance mass loss of metal-poor ($Z\leq 2.0\times 10^{-3}$) stars with ZAMS mass $60\leq $M$_{\mathrm{ZAMS}}/$M$_{\odot{}}\leq 125$. In contrast, PISNe become effective only for moderately metal-poor ($Z<8.0\times 10^{-3}$) VMSs. VMSs with M$_{\rm ZAMS}\gtrsim{}220$ M$_\odot$ and $Z<10^{-3}$ do not undergo PISNe and form intermediate-mass BHs (IMBHs, with mass $\gtrsim 200 $M$_{\odot{}}$) via direct collapse.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ebf73da3a2bd5defc18e8e9cdde6cf7cb0e97e3f

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Citations in the corpus

Search for Gravitational Lensing Signatures in LIGO-Virgo Binary Black Hole Events (2019, background): “The upper mass limit is motivated by pulsational pair-instability supernova, which prevents the formation of stellar remnants with mass ∼ 50 − 150M (Spera & Mapelli 2017; Woosley 2017; Belczynski et al. 2016b; Heger & Woosley 2002).”
The cosmic merger rate of neutron stars and black holes (2018, background): “- Pulsational pair-instability and pair-instability SNe are included, according to Spera & Mapelli (2017) (see also Woosley 2017 and Giacobbo et al. 2018).”
The effect of the metallicity-specific star formation history on double compact object mergers (2019, result): “Abbott et al. (2018b) find that existing gravitational-wave detections show evidence for a maximum black hole mass of around ∼45 M , consistent with population synthesis studies such as Belczynski et al. (2016b), Spera & Mapelli (2017), and Stevenson et al. (2019).”
The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks (2018, methodology): “The treatment of SNe was also deeply revised: we have included pulsational pair instability and pair instability SNe as described in Spera & Mapelli (2017), and we have added two new prescriptions for iron core-collapse SNe: the delayed and the rapid models presented in Fryer et al. (2012) (see…”
The cosmic merger rate of stellar black hole binaries from the Illustris simulation (2017, methodology): “Finally, we added a formalism to account for pair-instability and pulsational pair-instability SNe, following Spera & Mapelli (2017) (see also Belczynski et al. 2016c; Woosley 2017).”
Merging black holes in young star clusters (2019, methodology): “We stress that BHs with mass >∼ 60 M are inside the mass gap expected from PISNe and PPISNe (Belczynski et al. 2016a; Woosley 2017; Spera & Mapelli 2017): they can form dynamically because of multiple mergers between stars.”
A Future Percent-level Measurement of the Hubble Expansion at Redshift 0.8 with Advanced LIGO (2019, background): “A possible explanation for this drop is the pair instability supernova (PISN) process (Fowler & Hoyle 1964; Rakavy et al. 1967; Bond et al. 1984; Heger & Woosley 2002; Belczynski et al. 2016; Woosley 2017; Spera & Mapelli 2017; Leung et al. 2019).”
Merging black hole binaries with the SEVN code (2018, methodology): “Thus, from single stellar evolution, we do not expect to form BHs with mass 60 M (Spera & Mapelli 2017).”
Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo (2018, background): “Predictions for the maximum mass of BHs born after pulsational pair-instability supernovae are ∼50 M (Belczynski et al. 2016a; Spera & Mapelli 2017).”
Where Are LIGO’s Big Black Holes? (2017, background): “However, stars with MZAMS & 200M in a sufficiently lowmetallicity environment (Z∼ 0.07Z ) are expected to directly collapse to BHs with masses∼ 120–280M (Spera & Mapelli 2017).”
COSMIC Variance in Binary Population Synthesis (2019, methodology): “Prescription from Spera & Mapelli (2017) (see Ap- pendix B), which is derived from fitting the masses of the compact remnants as a function of the final Helium mass fraction and final helium core mass from the simulations in Woosley (2017).”
Modeling Dense Star Clusters in the Milky Way and Beyond with the CMC Cluster Catalog (2019, background): “…stellar mergers occurring through binary evolution may have important consequences for the formation of massive BHs, specifically BHs lying within the so-called upper mass gap expected from (pulsational) pair-instability SNe (e.g., Belczynski et al. 2016a; Woosley 2016; Spera & Mapelli 2017).”
Merging black hole binaries: the effects of progenitor's metallicity, mass-loss rate and Eddington factor (2017, methodology): “Currently, only few population-synthesis codes adopt up-to-date metallicity-dependent prescriptions for stellar winds (e.g. Belczynski et al. 2010; Toonen et al. 2012; Mapelli et al. 2013; Spera et al. 2015; Spera & Mapelli 2017; Banerjee 2017).”
Black hole growth through hierarchical black hole mergers in dense star clusters: implications for gravitational wave detections (2018, background): “Spera & Mapelli (2017) show that very massive stars with initial mass & 200M⊙ and Z 0.05Z⊙ form BHs with mass above & 200M⊙ via direct collapse.”