Tilted supercritical accretion disks around black holes can accrete mass at rates up to ten times the Eddington limit due to standing shocks, unlike untilted disks that respect the limit.
Title resolution pending
7 Pith papers cite this work, alongside 737 external citations. Polarity classification is still indexing.
7
Pith papers citing it
737
external citations · OpenAlex
years
2026 7representative citing papers
Milky Way globular clusters formed with initial half-mass densities of ~10^6.4 M_sun/pc^3, bottom-light IMFs, and small present-day black hole mass fractions, inferred by coupling rapid evolution models with multimass equilibrium models fitted to present-day observations.
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.
Two FRBs in the CHIME/FRB catalog look microlensed by black holes of roughly 550 and 2000 solar masses, presented as IMBH candidates.
ArkenstoneBH is a new subgrid model for the hot phase of black hole feedback that, in isolated galaxy tests, suppresses star formation by counteracting gas inflows from the circumgalactic medium.
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.
Reduces elliptic triple outcome model to one free parameter, matches N-body simulations except at low angular momentum, and finds observably eccentric merger fractions of 2.6-4.4% in 10^5-10^7 solar mass clusters.
citing papers explorer
-
The nature of tilted supercritical accretion discs
Tilted supercritical accretion disks around black holes can accrete mass at rates up to ten times the Eddington limit due to standing shocks, unlike untilted disks that respect the limit.
-
Fast Dynamical Modelling of Milky Way Globular Clusters -- I. Implications for Initial Cluster Densities
Milky Way globular clusters formed with initial half-mass densities of ~10^6.4 M_sun/pc^3, bottom-light IMFs, and small present-day black hole mass fractions, inferred by coupling rapid evolution models with multimass equilibrium models fitted to present-day observations.
-
From Dense Gas Clouds to Supermassive Black Hole Seeds: Hybrid Hydro/Direct $N$-body Simulations of Runaway Collision-driven Intermediate-mass Black Hole Formation
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.
-
Evidence for Intermediate-Mass Black Holes From Microlensing Signatures in CHIME/FRB catalog 2
Two FRBs in the CHIME/FRB catalog look microlensed by black holes of roughly 550 and 2000 solar masses, presented as IMBH candidates.
-
ArkenstoneBH. A model for high-specific energy black hole feedback in cosmological simulations
ArkenstoneBH is a new subgrid model for the hot phase of black hole feedback that, in isolated galaxy tests, suppresses star formation by counteracting gas inflows from the circumgalactic medium.
-
Binary Evolution Can Mimic the Pair-Instability Mass Gap in Black Hole Mergers
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.
-
Intermediate States in Chaotic Triple Evolution and Applications to Black Hole Merger Statistics
Reduces elliptic triple outcome model to one free parameter, matches N-body simulations except at low angular momentum, and finds observably eccentric merger fractions of 2.6-4.4% in 10^5-10^7 solar mass clusters.