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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D., Abraham, S., et al.2020
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A new redshift-correlation technique with third-generation GW detectors can constrain the BNS contribution to cosmic r-process nucleosynthesis to 5-6% precision via Fisher forecasts on mock bright- and dark-siren data.
AGN dust tori can form tens of millions of planetesimals from Earth to super-Jupiter masses via streaming instability, with continued growth to stellar masses through pebble and gas accretion.
Higher-order terms in an infinite tower of higher-derivative gravity regularize a 5D Proca-Maxwell system, creating frozen regular cores that mimic extremal black holes and satisfy all energy conditions.
Derives tight Holevo CRB for realistic linear sensors showing hierarchy with standard bounds and proposes readout improving LIGO rates by 25%.
N-body simulations demonstrate runaway GW BBH mergers in dense BH clusters (≥5×10^9 M⊙/pc³) produce ~10³ M⊙ IMBHs within 10 Myr.
Mass ratio reversals produce qualitatively different contributions to BBH merger rates and masses in COMPAS versus SEVN simulations, with core-growth dominating and most systems arising from massive low-metallicity progenitors.
Two FRBs exhibit microlensing signatures consistent with intermediate-mass black holes of masses approximately 500-600 and 1500-2500 solar masses, interpreted as possible evidence for isolated primordial black holes comprising about 4% of dark matter.
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.
Efficient mass transfer in binaries naturally limits the mass of the first-born black hole and produces a sharp drop above 45 solar masses that mimics the pair-instability gap.
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.
The chirp-mass distribution of GW-detected binary black holes shows a ladder of peaks doubling in mass, with a new intermediate peak at 19 solar masses confirming a prior prediction from the hierarchical merger model.
92% of 91 LIGO black hole mergers favor non-zero V_GW, constraining bound remnants to at most 8% and finding no cosmological handedness preference with average near zero.
Semi-analytical models show AGN disks produce repeated BBH mergers with a high-mass tail beyond the pair-instability gap, more efficiently at low viscosity, with spin and mass-ratio signatures that can match events like GW190521.
LILA can detect IMBH binaries at redshifts 20-30, IMRIs, and provide months-to-years early warnings with high-SNR events for gravity tests.
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.
No evidence for core-collapse formed low-spin IMBHs in GWTC-4, with 90% upper limit on merger rate of 0.077 Gpc^{-3} yr^{-1}, low-spin BH mass truncation at 65 solar masses consistent with pair-instability gap lower edge, and high-spin IMBHs from hierarchical mergers.
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.
Cosmic Explorer is described as a next-generation gravitational-wave observatory aiming for tenfold sensitivity improvement over Advanced LIGO to observe signals from the edge of the observable universe at z~100.
High-metallicity star cluster simulations produce black hole mergers with masses and ratios consistent with recent LVK detections, unlike low-metallicity models.
Simulations show LIGO-A# constrains the peak redshift of binary black hole merger rate (tracing star formation) to ±0.1 in one year, improving to ±0.02 with next-generation detectors.
Simulations show VMS in star clusters reach 10^3-10^4 solar masses with dimensionless spins >10 under bloated accretion conditions, potentially forming spinning IMBHs that produce GW bursts like GW190521.
Modeling of jets escaping AGN disks reveals distinct nonthermal emission signatures that support multi-messenger detection and diagnostics of the AGN environment.
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Rapid intermediate-mass black hole formation via runaway mergers of black holes
N-body simulations demonstrate runaway GW BBH mergers in dense BH clusters (≥5×10^9 M⊙/pc³) produce ~10³ M⊙ IMBHs within 10 Myr.
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AGN-driven BBH mergers: Black hole populations and hierarchical growth across the AGN parameter space
Semi-analytical models show AGN disks produce repeated BBH mergers with a high-mass tail beyond the pair-instability gap, more efficiently at low viscosity, with spin and mass-ratio signatures that can match events like GW190521.
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