Polarization angle swings in photons near a Kerr black hole during ringdown lock in time to quasi-normal modes with amplitudes up to about 10 degrees.
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Autocorrelation signatures in time-resolved black hole flare images: Secondary peaks and convergence structure
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Corotating point sources on accretion disks near black holes distort the relative magnification factor distribution, modulating caustics and encoding accretion flow kinematics via time-delayed images.
Fitting GRAVITY flare astrometry to solitonic boson star models requires masses larger than 4.3 million solar masses, with more diffuse models yielding values closer to the standard black hole mass and thus placing stringent but incomplete constraints on such interpretations of Sgr A*.
Bayesian fitting to mock GRAVITY data shows robust detection of secondary images from Sgr A* flares requires both an order-of-magnitude larger sample and astrometric uncertainties reduced to 40% of current levels for |ΔBIC| > 7.9.
Bayesian analysis shows current near-IR astrometry data cannot distinguish massive boson stars from Schwarzschild black holes for Sgr A*.
Increasing charge Q shrinks photon rings and central shadows in Kerr-Sen black hole images while spin creates brightness asymmetry; polarization patterns follow lensing and frame dragging.
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