Synchrotron polarization at the black hole horizon follows a universal pattern set solely by spin and inclination.
and Lupsasca, Alexandru
9 Pith papers cite this work. Polarity classification is still indexing.
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Scalarized Kerr-Newman black holes develop an inner photon shell that produces an additional critical curve and distinct crescent-like higher-order images unlike those in Kerr spacetime.
Steady GRMHD jets exhibit a universal near-horizon polarization pattern set only by black hole spin, with large-radius polarization angle following a collimation-determined power law and intermediate scales modified by plasma loading.
Machine learning on simulated images identifies that flux eruption events cause more diffuse, polarized, lower-flux millimeter emission with decreased Q-U loop rotation rate, achieving ~80% accuracy with random forests on summary statistics.
Simulations show the singularity-free Kerr-Hayward metric yields EHT observables that are functionally indistinguishable from the Kerr metric.
Simulations of accreting black holes in standard and complex spacetimes indicate that magnetic geometry, quantum corrections, and binary dynamics influence flares, precession, photon rings, and multi-wavelength variability, with potential EHT constraints.
EHT angular diameter data yield upper bounds on the holonomy correction b (e.g., b ≤ 0.1319M at a=0 for M87*) showing nonzero b remains consistent with observations for RHCBH spacetimes.
GRMHD simulations at spins 0.9375 and 0.998 yield similar fluid properties and full-Stokes EHT images, indicating prior lower-spin runs remain representative for a ≳ 0.9375.
GRRT simulations show that raising the dilaton parameter shrinks the bright ring while increasing its width and brightness, disk thickness reduces diameter and width with weaker brightness impact, and both affect allowed ranges versus EHT Sgr A* data and the polarization coefficient beta2.
citing papers explorer
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Black Hole Polarimetry III: Universal Polarization of Synchrotron Radiation at the Horizon
Synchrotron polarization at the black hole horizon follows a universal pattern set solely by spin and inclination.
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Optical Appearance of Scalarized Kerr-Newman Black Holes with Multiple Light Rings
Scalarized Kerr-Newman black holes develop an inner photon shell that produces an additional critical curve and distinct crescent-like higher-order images unlike those in Kerr spacetime.
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Polarization Architecture of Steady GRMHD Jets from the Horizon to Infinity
Steady GRMHD jets exhibit a universal near-horizon polarization pattern set only by black hole spin, with large-radius polarization angle following a collimation-determined power law and intermediate scales modified by plasma loading.
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Identifying Observational Signatures of Flux Eruption Events in Supermassive Black Hole Accretion Flows with Machine Learning
Machine learning on simulated images identifies that flux eruption events cause more diffuse, polarized, lower-flux millimeter emission with decreased Q-U loop rotation rate, achieving ~80% accuracy with random forests on summary statistics.
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On the observational distinguishability of the Kerr and Kerr-Hayward metrics to EHT
Simulations show the singularity-free Kerr-Hayward metric yields EHT observables that are functionally indistinguishable from the Kerr metric.
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GRMHD and GRRT Simulations of Black Hole Accretion: Flares, Precession, and Complex Spacetimes
Simulations of accreting black holes in standard and complex spacetimes indicate that magnetic geometry, quantum corrections, and binary dynamics influence flares, precession, photon rings, and multi-wavelength variability, with potential EHT constraints.
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Testing loop quantum gravity through EHT observations of M87* and Sgr A* using rotating holonomy-corrected black holes
EHT angular diameter data yield upper bounds on the holonomy correction b (e.g., b ≤ 0.1319M at a=0 for M87*) showing nonzero b remains consistent with observations for RHCBH spacetimes.
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Observational Properties of Near-Maximally Spinning Supermassive Black Holes
GRMHD simulations at spins 0.9375 and 0.998 yield similar fluid properties and full-Stokes EHT images, indicating prior lower-spin runs remain representative for a ≳ 0.9375.
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Bright ring features and polarization structures in Kerr-Sen black hole images illuminated by radiatively inefficient accretion flows
GRRT simulations show that raising the dilaton parameter shrinks the bright ring while increasing its width and brightness, disk thickness reduces diameter and width with weaker brightness impact, and both affect allowed ranges versus EHT Sgr A* data and the polarization coefficient beta2.