Three observables on a standardized segment of the Kerr critical curve uniquely fix spin a/M, inclination i, and segment location r_nl within the considered domain.
Kocherlakota et al
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Kerr-MOG accretion disk spectra are softer than Kerr at fixed spin due to outward ISCO shift from the fifth-force parameter α, with an observational upper limit α < 0.044 from LMC X-1 data.
Simulations show the singularity-free Kerr-Hayward metric yields EHT observables that are functionally indistinguishable from the Kerr metric.
Numerical geodesics show narrow deflection angles for massive particle scattering off RN black holes versus isotropic scattering off naked singularities.
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.
Increasing the asymptotic safety parameter and spin shrinks the shadow size while increasing its distortion for a rotating Bardeen black hole, with monopole charge shaping the profile and energy emission rates also computed.
citing papers explorer
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Determining Kerr black hole spin and inclination from a segment of the critical curve in black hole images
Three observables on a standardized segment of the Kerr critical curve uniquely fix spin a/M, inclination i, and segment location r_nl within the considered domain.
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Scattering of massive particles from black holes and naked singularities
Numerical geodesics show narrow deflection angles for massive particle scattering off RN black holes versus isotropic scattering off naked singularities.
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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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EHT-Constrained Analysis of Shadow Deformation in Quantum-Improved Rotating Non-Singular Magnetic Monopole
Increasing the asymptotic safety parameter and spin shrinks the shadow size while increasing its distortion for a rotating Bardeen black hole, with monopole charge shaping the profile and energy emission rates also computed.