Observations and modeling of SN 2023vbw indicate it is a pair-instability supernova with ejecta mass 170-350 solar masses, nickel mass 1.2-1.6 solar masses, and explosion energy (6-13) x 10^52 erg.
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GWTC-4 data reveals a pair-instability gap at 44 M_⊙ in secondary black hole masses, interpreted as evidence for hierarchical mergers and used to constrain the S-factor for 12C(α,γ)16O.
Streaming instability in magnetized AGN dust tori can yield tens of millions of planetary-mass objects per AGN, some formed directly above the hydrogen-burning limit.
Monte Carlo simulations of AGN-disk black hole mergers identify dense, moderately short-lived disks, a steep initial mass function, and mostly prograde orbits as the parameter combination that reproduces the observed (q, χ_eff) anti-correlation.
citing papers explorer
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The pair-instability origin of supernova 2023vbw
Observations and modeling of SN 2023vbw indicate it is a pair-instability supernova with ejecta mass 170-350 solar masses, nickel mass 1.2-1.6 solar masses, and explosion energy (6-13) x 10^52 erg.
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Evidence of the pair instability gap from black hole masses
GWTC-4 data reveals a pair-instability gap at 44 M_⊙ in secondary black hole masses, interpreted as evidence for hierarchical mergers and used to constrain the S-factor for 12C(α,γ)16O.
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Active Galactic Nucleus Tori: Potential Birthplace to Millions of Planets
Streaming instability in magnetized AGN dust tori can yield tens of millions of planetary-mass objects per AGN, some formed directly above the hydrogen-burning limit.
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McFACTS II: Mass Ratio--Effective Spin Relationship of Black Hole Mergers in the AGN Channel
Monte Carlo simulations of AGN-disk black hole mergers identify dense, moderately short-lived disks, a steep initial mass function, and mostly prograde orbits as the parameter combination that reproduces the observed (q, χ_eff) anti-correlation.