An exact analytic metric is constructed for rotating black holes embedded in generic dark matter halos with a central density spike that vanishes beyond a truncation radius near the horizon, generalizing prior spherical solutions.
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The Core-Cusp Problem
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abstract
This paper gives an overview of the attempts to determine the distribution of dark matter in low surface brightness disk and gas-rich dwarf galaxies, both through observations and computer simulations. Observations seem to indicate an approximately constant dark matter density in the inner parts of galaxies, while cosmological computer simulations indicate a steep power-law-like behaviour. This difference has become known as the "core/cusp problem", and remains one of the unsolved problems in small-scale cosmology.
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Non-equilibrium relativistic SIDM halo collapse produces seed black holes of mass ~3e-8 of the halo mass at apparent horizon formation.
No three-body encounter signatures detected in GW170817, GW190814, and GW230627_015337, constraining intermediate-mass black holes above 100 solar masses within roughly 0.1 AU of these binaries.
Self-interacting dark matter increases the Euler characteristic of the reionization ionization field by 60-70% for cross-sections above 2 cm2/g through changes in ionizing source populations.
Empirical three-parameter fit to f_esc(M_h,z) yields steep redshift evolution with population-averaged escape fraction rising from ~2% at z=5 to ~9% at z=12.
A scalar-mediated inelastic dark matter model with 100 eV splitting, Z2 symmetry forbidding elastic scattering, and a dimension-5 dipole operator reconciles dwarf galaxy observations with cosmological bounds via resonant enhancement and provides a distinct direct detection signal.
Super-resonant dark matter at O(100) GeV masses amplifies self-scattering and annihilation cross sections via combined resonance and Sommerfeld effects, necessitating coupled Boltzmann equations to match observed relic density.
Degeneracy-induced depletion from fermionic DM in subhalos creates structure-wide low-density cores consistent with observations, linking profile diversity to formation history.
21 cm reionization topology breaks the degeneracy between self-interacting dark matter and astrophysical parameters that limits UV luminosity function constraints, enabling robust SIDM limits of σ/m ≳ 1-2 cm²/g independent of star formation models.
Core-collapsed SIDM halos produce longer FRB image time delays than CDM halos, enabling future surveys to constrain self-interaction cross sections above roughly 18-40 cm²/g depending on collapse timing.
In TNG50, compact dwarf satellites (log M_star 8.4-9.2) form via DM-rich gas inflows in low-merger environments, tidal stripping for DM-poor cases, and ram-pressure starbursts for some metal-rich ones.
Simulations show fuzzy dark matter fraction up to 0.3 suppresses low-mass halos in mixed DM models, and a redshift- and fraction-dependent suppression function maps CDM HMFs to MDM HMFs within 0.1-0.2 dex accuracy for z=1-4.
Dark matter halo profiles admit effective nonlinear electrodynamics completions that source regular black holes exhibiting de Sitter cores for finite central density and Schwarzschild asymptotics.
Null detection of extra lensed images in 3500 mock systems constrains PBH abundance to ≲0.04-0.125% and excludes FDM masses below 0.4-3.5×10^{-22} eV at 95% CL depending on angular resolution.
Dynamical friction from a degenerate fermionic dark matter background induces measurable secular decay in binary pulsar orbital periods, with sensitivity to fermion masses ≳50 eV and example upper bounds around 1 keV from Milky Way data.
Five of seven modeled M31 dwarf spheroidals show anomalously low central DM densities at 150 pc, with star formation heating disfavored as the sole cause.
Fuzzy dark matter with smooth cored halos provides the most consistent description of M31's rotation curve among scalar field models when paired with a two-bulge baryonic configuration.
Review of state-of-the-art cosmological galaxy formation models for HI, molecular gas and radio continuum in preparation for SKA, advocating coordinated multi-scale simulations, forward modelling and AI emulators.
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Constraining light fermionic dark matter with binary pulsars
Dynamical friction from a degenerate fermionic dark matter background induces measurable secular decay in binary pulsar orbital periods, with sensitivity to fermion masses ≳50 eV and example upper bounds around 1 keV from Milky Way data.