A new gravitational wave event reveals a binary black hole merger with total mass 190-265 solar masses, indicating black holes can form via gravitational-wave driven mergers beyond standard stellar channels.
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Eccentricity posteriors of dynamically captured binaries can be mapped to capture parameters and compared against environment velocity distributions to constrain host and infer decay time.
Mixture model analysis of LIGO data identifies a ~10% high-spin subpopulation with a1 ≈ 0.9 matching AGN accretion predictions, disfavoring hierarchical mergers at a1 ≈ 0.7 for that group.
Ground-triggered Bayesian analysis enables detection and tight constraints on eccentricity and chirp mass for a GW190521-like eccentric binary black hole in one year of LISA or TianQin data at SNR ~7.
Updated ANC constraints on the 12C(alpha,gamma)16O S-factor favor lower values than prior evaluations and imply a black-hole mass-gap lower edge of 61-75 solar masses.
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.
Isolated Population III binaries can form GW231123-like events if convective overshooting is inefficient, the carbon-alpha reaction rate is 2 sigma below standard, and initial orbits match those of later-generation binaries.
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.
The paper computes the graviton-scalar Compton scattering cross section via EFT at ~30 PeV center-of-mass energy and derives an impact parameter that, after coherence enhancement, scales with the known LIGO GW strain and mirror recoil.
citing papers explorer
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GW231123: a Binary Black Hole Merger with Total Mass 190-265 $M_{\odot}$
A new gravitational wave event reveals a binary black hole merger with total mass 190-265 solar masses, indicating black holes can form via gravitational-wave driven mergers beyond standard stellar channels.
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Inferring host environment properties and gravitational-wave decay time from the eccentricity measurement of dynamically captured binaries
Eccentricity posteriors of dynamically captured binaries can be mapped to capture parameters and compared against environment velocity distributions to constrain host and infer decay time.
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High-Spin BBH Subpopulation from AGN Accretion
Mixture model analysis of LIGO data identifies a ~10% high-spin subpopulation with a1 ≈ 0.9 matching AGN accretion predictions, disfavoring hierarchical mergers at a1 ≈ 0.7 for that group.
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Archival Inference for Eccentric Stellar-Mass Binary Black Holes in Space-Based Gravitational Wave Observations
Ground-triggered Bayesian analysis enables detection and tight constraints on eccentricity and chirp mass for a GW190521-like eccentric binary black hole in one year of LISA or TianQin data at SNR ~7.
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Nuclear Constraints on $^{12}$C$(\alpha,\gamma)^{16}$O and Their Impact on Black-Hole Mass Predictions
Updated ANC constraints on the 12C(alpha,gamma)16O S-factor favor lower values than prior evaluations and imply a black-hole mass-gap lower edge of 61-75 solar masses.
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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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GW231123 Formation from Population III Stars: Isolated Binary Evolution
Isolated Population III binaries can form GW231123-like events if convective overshooting is inefficient, the carbon-alpha reaction rate is 2 sigma below standard, and initial orbits match those of later-generation binaries.
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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.
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Effective Field Theory Calculation of LIGO-like Compton Scattering
The paper computes the graviton-scalar Compton scattering cross section via EFT at ~30 PeV center-of-mass energy and derives an impact parameter that, after coherence enhancement, scales with the known LIGO GW strain and mirror recoil.