Binary interactions and cluster dynamics boost PISN rates by up to 3x versus single stars, enabling constraints on stellar-wind mass loss and galaxy metallicity distributions.
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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.
Direct collapse black holes born at z=25.7 grow at half-Eddington rate to produce overmassive black hole galaxies at z~10 with M_BH/M_* ~0.01, matching JWST observations of GN-z11, UHZ1, and GHZ9 through initial star-formation suppression and later Pop III supernova metal blowout.
Cavity truncation in circumbinary discs is set by binary parameters together with instantaneous cavity eccentricity and relative apsidal orientation, yielding a prescription for pericentre radius Rp and semi-major axis acav.
Hybrid hydro/direct N-body simulations of dense high-redshift gas clouds form very massive stars via runaway collisions that collapse to IMBHs capable of growing from ~6700 to ~62000 solar masses in 100 Myr under optimistic assumptions.
NEFERTITI simulations show that the Milky Way's most metal-poor stars largely come from a handful of accreted massive dwarf galaxies, while reproducing the JWST Hebe galaxy at z~11 as a pure Population III system.
A pair-instability supernova from a 250-260 solar mass Population III star at z≈15 matches the brightness, variability, photometry, and spectrum of the JWST source Capotauro.
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.
The MAGIC survey provides photometric metallicities for RGB stars over ~3000 deg² using CaHK narrow-band imaging plus DELVE g,r,i data, recovering 13/14 known ultra-faint dwarfs and confirming a distant Reticulum II member.
Super-Eddington accretion boosts predicted LISA detections of high-redshift black hole binaries to ~64 per year while dropping ET detections to ~4 per year, compared to ~32 and ~64 under Eddington-limited growth.
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.
Jet-driven aspherical explosions improve fits to Perseus Cluster abundances and are necessary to explain zinc enrichment and other elemental trends in galactic stars and chemical evolution models.
New CCSN yield tables at varying metallicities are inserted into galactic chemical evolution models and tuned to reproduce the Si-group and Fe-group abundances measured by Hitomi in the Perseus Cluster.
SLSN 2021bnw is best fit by a core-collapse explosion of a star with initial mass at least 61 solar masses, ejecta of 15-22.5 solar masses containing 1.7 solar masses of nickel-56 and 4 foe energy colliding with 7 solar masses of circumstellar matter.
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.
Slowly rotating 80-85 solar mass Pop III stars form black holes of similar mass with dimensionless spins up to 0.7, just below the pair-instability gap.
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.
Intermediate-mass black holes acting as permanent matter sinks, combined with updated cosmic star formation rates and primordial baryon accretion, reduce the overpredicted CNO abundances from Population III stars to match observations in z~3-6 quasar absorption systems.