The upper edge of the PISN black hole mass gap shifts by up to 30 solar masses due to nuclear reaction rate uncertainties, primarily the 12C(α,γ)16O rate, while remaining robust to resolution variations unlike the lower edge.
Resolving the Peak of the Black Hole Mass Spectrum
6 Pith papers cite this work. Polarity classification is still indexing.
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New MESA stellar tracks with varied winds and convective mixing produce a primary black hole mass function with twin peaks near 8 and 13 solar masses in most variations, the higher peak dominated by mass-ratio-reversal systems, with rates varying by a factor of six.
Slowly rotating 80–85 M☉ Pop III stars can keep most of their mass and form black holes with spins up to a_BH ≲ 0.7 just below the pair-instability gap.
Stellar models show that the 12C(alpha,gamma)16O rate uncertainty moves the black hole mass gap, constraining its S300 to 137.6-263.4 keV barn when matched to the observed gap from gravitational waves.
New 17O+α and 22Ne+α rates increase weak s-process yields by tens of times in Z=10^{-3} stars of 15-30 solar masses.
citing papers explorer
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The location of the upper edge of the pair-instability supernovae black hole mass gap
The upper edge of the PISN black hole mass gap shifts by up to 30 solar masses due to nuclear reaction rate uncertainties, primarily the 12C(α,γ)16O rate, while remaining robust to resolution variations unlike the lower edge.
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Twin Peaks: Resolving Features in the Binary Black Hole Mass Function with COSMIC-METISSE
New MESA stellar tracks with varied winds and convective mixing produce a primary black hole mass function with twin peaks near 8 and 13 solar masses in most variations, the higher peak dominated by mass-ratio-reversal systems, with rates varying by a factor of six.
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Fast-spinning massive black holes from slowly rotating low-metallicity stars: Implications for GW231123
Slowly rotating 80–85 M☉ Pop III stars can keep most of their mass and form black holes with spins up to a_BH ≲ 0.7 just below the pair-instability gap.
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Constraints on the $^{12}$C$(\alpha, \gamma)^{16}$O and $^{16}$O+$^{16}$O Reaction Rates from Binary Black Holes Detected via Gravitational Wave Signals
Stellar models show that the 12C(alpha,gamma)16O rate uncertainty moves the black hole mass gap, constraining its S300 to 137.6-263.4 keV barn when matched to the observed gap from gravitational waves.
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The impact of new ($\alpha$, n) reaction rates on the weak s-process in metal-poor massive stars
New 17O+α and 22Ne+α rates increase weak s-process yields by tens of times in Z=10^{-3} stars of 15-30 solar masses.
- Mass and Spin Growth of Very Massive Stars in Star Clusters Potentially Associated with Little Red Dots