The Effect of Supernova Convection On Neutron Star and Black Hole Masses

Fryer, Chris L.; Olejak, Aleksandra; Belczyński, Krzysztof

doi:10.3847/1538-4357/ac6ac9

Cited by 41 publications

(32 citation statements)

References 86 publications

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“…This gives an upper limit in the initial BH mass function of about 50M . However, there are several uncertainties in the modelling, and different assumptions can lead to significantly different values for the high mass cut-off, generally in the range 40M to 70M (Giacobbo et al 2018;Farmer et al 2020;Costa et al 2021;Fryer et al 2022). Exploring the effect of these uncertainties is beyond the scope of this paper, but should be considered in future work.…”

Section: Discussionmentioning

confidence: 99%

Coalescing black hole binaries from globular clusters: mass distributions and comparison to gravitational wave data from GWTC-3

Antonini¹,

Gieles²,

Dosopoulou³

et al. 2022

Preprint

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We use our cluster population model, cBHBd, to explore the mass distribution of merging black hole binaries formed dynamically in globular clusters. We include in our models the effect of mass growth through hierarchical mergers and compare the resulting distributions to those inferred from the third gravitational wave transient catalogue. We find that none of our models can reproduce the peak at m 1 10M in the primary black hole mass distribution that is inferred from the data. This disfavours a scenario where most of the detected sources are formed in globular clusters. On the other hand, a globular cluster origin can account for the inferred secondary peak at m 1 35M , which requires that the most massive clusters form with half-mass densities ρ h,0 10 4 M pc −3 . Finally, we find that the lack of a high mass cut-off in the inferred mass distribution can be also explained by the repopulation of an initial mass gap through hierarchical mergers. Matching the inferred merger rate above 50M requires both initial cluster densities ρ h,0 10 4 M pc −3 , and that black holes form with nearly zero spin. A hierarchical merger scenario makes specific predictions for the appearance and position of multiple peaks in the black hole mass distribution, which can be tested against future data.

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Section: Discussionmentioning

confidence: 99%

Coalescing black hole binaries from globular clusters: mass distributions and comparison to gravitational wave data from GWTC-3

Antonini¹,

Gieles²,

Dosopoulou³

et al. 2022

Preprint

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show abstract

“…The "lower edge" of the lower mass gap is set by the maximum possible neutron star mass, while the "upper edge" is set by the minimum observed BH mass. The upper edge of the lower mass gap, if it exists, is currently uncertain, as the BHs found in this mass range may have been created by changes in the growth time of convection during an SN explosion (Fryer et al 2022) or by binary neutron star mergers (Thompson et al 2019;Abbott et al 2020;Gupta et al 2020;Yang et al 2020;Ye & Fishbach 2022).…”

Section: Introductionmentioning

confidence: 99%

“…A number of uncertain factors make a straightforward determination challenging. For example, current estimates of the BH initial mass function from single stars chiefly rely on parameterized explosion models (Fryer et al 2012;Spera et al 2015;Patton & Sukhbold 2020;Zapartas et al 2021;Fryer et al 2022;Patton et al 2022;Renzo et al 2022). Models for the evolution from the ZAMS also still rely on effective mixing length theories for convection, including ours.…”

Section: Introductionmentioning

confidence: 99%

Resolving the Peak of the Black Hole Mass Spectrum

Farag

Renzo

Farmer

et al. 2022

ApJ

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Gravitational-wave (GW) detections of binary black hole (BH) mergers have begun to sample the cosmic BH mass distribution. The evolution of single stellar cores predicts a gap in the BH mass distribution due to pair-instability supernovae (PISNe). Determining the upper and lower edges of the BH mass gap can be useful for interpreting GW detections of merging BHs. We use MESA to evolve single, nonrotating, massive helium cores with a metallicity of Z = 10−5, until they either collapse to form a BH or explode as a PISN, without leaving a compact remnant. We calculate the boundaries of the lower BH mass gap for S-factors in the range S(300 keV) = (77,203) keV b, corresponding to the ±3σ uncertainty in our high-resolution tabulated 12C(α,γ)16O reaction rate probability distribution function. We extensively test temporal and spatial resolutions for resolving the theoretical peak of the BH mass spectrum across the BH mass gap. We explore the convergence with respect to convective mixing and nuclear burning, finding that significant time resolution is needed to achieve convergence. We also test adopting a minimum diffusion coefficient to help lower-resolution models reach convergence. We establish a new lower edge of the upper mass gap as M lower ≃ 60 − 14 + 32 M ⊙ from the ±3σ uncertainty in the 12C(α, γ)16O rate. We explore the effect of a larger 3α rate on the lower edge of the upper mass gap, finding M lower ≃ 69 − 18 + 34 M ⊙. We compare our results with BHs reported in the Gravitational-Wave Transient Catalog.

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“…The "lower edge" of the lower mass gap is set by the maximum possible neutron star mass while the "upper edge" is set by the minimum observed BH mass. The upper edge of the lower mass gap, if it exists, is currently uncertain as BHs found in this mass range may have been created by changes in the growth time of convection during a SN explosion (Fryer et al 2022), or by binary neutron star mergers (Thompson et al 2019;Abbott et al 2020;Gupta et al 2020;Yang et al 2020;Ye & Fishbach 2022).…”

Section: Introductionmentioning

confidence: 99%

“…A number of uncertain factors make a straightforward determination challenging. For example, current estimates of the BH initial mass function from single stars chiefly rely on parameterized explosion models (Spera et al 2015;Patton & Sukhbold 2020;Zapartas et al 2021;Patton et al 2022;Fryer et al 2012Fryer et al , 2022Renzo et al 2022). Models for the evolution from the ZAMS also still rely on effective mixing length theories for convection, including ours.…”

Section: Introductionmentioning

confidence: 99%

Resolving The Peak Of The Black Hole Mass Spectrum

Farag

Renzo

Farmer

et al. 2022

View full text Add to dashboard Cite

Gravitational wave (GW) detections of binary black hole (BH) mergers have begun to sample the cosmic BH mass distribution. The evolution of single stellar cores predicts a gap in the BH mass distribution due to pair-instability supernova (PISN). Determining the upper and lower edges of the BH mass gap can be useful for interpreting GW detections from merging BHs. We use MESA to evolve single, non-rotating, massive helium cores with a metallicity of Z = 10 −5 until they either collapse to form a BH or explode as a PISN without leaving a compact remnant. We calculate the boundaries of the lower BH mass gap for S-factors in the range S(300 keV) = (77,203) keV b, corresponding to the ±3σ uncertainty in our high resolution tabulated 12 C(α,γ) 16 O reaction rate probability distribution function. We extensively test the temporal and mass resolution to resolve the theoretical peak of the BH mass spectrum across the BH mass gap. We explore the convergence with respect to convective mixing and nuclear burning, finding that significant time resolution is needed to achieve convergence. We also test adopting a minimum diffusion coefficient to help lower resolution models reach convergence. We establish a new lower edge of the upper mass gap as M lower 60 +32 −14 M from the ±3σ uncertainty in the 12 C(α, γ) 16 O rate. We explore the effect of a larger 3-α rate on the lower edge of the upper mass gap, finding M lower 69 +34 −18 M . We compare our results with BHs reported in the Gravitational-Wave Transient Catalog.

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The Effect of Supernova Convection On Neutron Star and Black Hole Masses

Cited by 41 publications

References 86 publications

Coalescing black hole binaries from globular clusters: mass distributions and comparison to gravitational wave data from GWTC-3

Coalescing black hole binaries from globular clusters: mass distributions and comparison to gravitational wave data from GWTC-3

Resolving the Peak of the Black Hole Mass Spectrum

Resolving The Peak Of The Black Hole Mass Spectrum

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