Cuspy black hole shadows correspond to swallowtail thermodynamic free energy, with boundary self-intersections marking geometric phase transitions whose critical exponents fall in the mean-field class.
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Entropy corrections to black holes produce modified metrics whose photon-sphere and shadow sizes can be constrained by Sgr A* observations.
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.
Hairy black hole shadows and disks grow with horizon scalar value but can mimic Schwarzschild by adjusting horizon radius, with the potential parameter Lambda constrained by supermassive black hole observations.
citing papers explorer
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Gravity/thermodynamics correspondence via black hole shadows
Cuspy black hole shadows correspond to swallowtail thermodynamic free energy, with boundary self-intersections marking geometric phase transitions whose critical exponents fall in the mean-field class.
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Photon Spheres and shadow of modified black-hole entropies
Entropy corrections to black holes produce modified metrics whose photon-sphere and shadow sizes can be constrained by Sgr A* observations.
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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.
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Shadow of the Scalar Hairy Black Hole with Inverted Higgs Potential
Hairy black hole shadows and disks grow with horizon scalar value but can mimic Schwarzschild by adjusting horizon radius, with the potential parameter Lambda constrained by supermassive black hole observations.