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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10 Pith papers cite this work. Polarity classification is still indexing.
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Detection of GW190814 from the coalescence of a 23 solar-mass black hole and a 2.6 solar-mass compact object, the most unequal-mass binary yet observed with gravitational waves.
Introduces a frequentist p-value approach to falsify models of binary black hole formation for events such as GW190521, showing some models are adequate while others are not.
LILA can detect IMBH binaries at redshifts 20-30, IMRIs, and provide months-to-years early warnings with high-SNR events for gravity tests.
Coupled cosmological and cluster simulations show isolated binary evolution cannot produce GW231123-like mergers at the observed redshift, while hierarchical mergers in globular clusters can, yielding a local rate of 0.78 Gpc^{-3} yr^{-1} peaking at z=4-6.
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.
Self-interacting dark matter with particle mass m ≳ 0.01 eV drives universal super-Eddington Bondi accretion that grows 10 solar-mass primordial black holes into 10^9-10^10 solar-mass supermassive black holes by z~7.
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.
N-body models of young and old dense star clusters show BBH mergers span primary masses from ~6 to >100 solar masses with a peak near 8 solar masses, reproducing the LIGO-inferred distribution, with low-mass mergers mostly from metal-rich clusters.
No model-independent evidence for a peak in binary black hole spin tilts is found in GWTC-4; mass-spin magnitude correlation is confirmed but mass-tilt correlation is not.
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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GW190814: Gravitational Waves from the Coalescence of a 23 M$_\odot$ Black Hole with a 2.6 M$_\odot$ Compact Object
Detection of GW190814 from the coalescence of a 23 solar-mass black hole and a 2.6 solar-mass compact object, the most unequal-mass binary yet observed with gravitational waves.
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Are all models wrong? Falsifying binary formation models in gravitational-wave astronomy
Introduces a frequentist p-value approach to falsify models of binary black hole formation for events such as GW190521, showing some models are adequate while others are not.
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Black Hole Binary Detection Landscape for the Laser Interferometer Lunar Antenna (LILA): Signal-to-Noise Calculations & Science Cases
LILA can detect IMBH binaries at redshifts 20-30, IMRIs, and provide months-to-years early warnings with high-SNR events for gravity tests.
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Investigating the formation channel of GW231123: Population III stars or hierarchical mergers?
Coupled cosmological and cluster simulations show isolated binary evolution cannot produce GW231123-like mergers at the observed redshift, while hierarchical mergers in globular clusters can, yielding a local rate of 0.78 Gpc^{-3} yr^{-1} peaking at z=4-6.
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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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A Unified Dark-Matter--Driven Relativistic Bondi Route to Black-Hole Growth from Stellar to Supermassive Scales
Self-interacting dark matter with particle mass m ≳ 0.01 eV drives universal super-Eddington Bondi accretion that grows 10 solar-mass primordial black holes into 10^9-10^10 solar-mass supermassive black holes by z~7.
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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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Mass Distribution of Binary Black Hole Mergers from Young and Old Dense Star Clusters
N-body models of young and old dense star clusters show BBH mergers span primary masses from ~6 to >100 solar masses with a peak near 8 solar masses, reproducing the LIGO-inferred distribution, with low-mass mergers mostly from metal-rich clusters.
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No model-independent evidence for a peak in binary black hole spin (mis)alignments
No model-independent evidence for a peak in binary black hole spin tilts is found in GWTC-4; mass-spin magnitude correlation is confirmed but mass-tilt correlation is not.