In dRGT massive gravity, static spherically symmetric black holes exhibit zero, one, or two photon spheres whose topological charges and stability patterns differ from Einstein gravity and from horizonless compact objects.
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The geometry of photon surfaces
Mixed citation behavior. Most common role is background (67%).
15
Pith papers citing it
Background
67% of classified citations
abstract
The photon sphere concept in Schwarzschild space-time is generalized to a definition of a photon surface in an arbitrary space-time. A photon sphere is then defined as an SO(3)xR-invariant photon surface in a static spherically symmetric space-time. It is proved, subject to an energy condition, that a black hole in any such space-time must be surrounded by a photon sphere. Conversely, subject to an energy condition, any photon sphere must surround a black hole, a naked singularity or more than a certain amount of matter. A second order evolution equation is obtained for the area of an SO(3)-invariant photon surface in a general non-static spherically symmetric space-time. Many examples are provided.
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representative citing papers
Exact static vacuum solution in Einstein-Aether theory parameterized by c14, with analytic extension showing naked singularities or wormhole geometries rather than black holes when c14 is nonzero.
In general LTB dust collapse the photon surface is a null hypersurface generated by outgoing radial null geodesics that reaches the central singularity if and only if the singularity is naked.
Analytic perturbative black hole solutions in dark photon models with minimal and higher-order magnetic dipole corrections to the Schwarzschild geometry.
An invariant function is derived whose zeros identify spherical photon orbits in Kerr spacetime, parameterized by an inclination angle, enabling invariant characterization of the photon region and constants of motion.
A reference-renormalized curvature-primitive Gauss-Bonnet formalism computes finite-distance weak deflection angles in static spherical spacetimes without invoking photon spheres.
Presents a curvature-based perturbative method for photon spheres, massive particle surfaces, and black hole shadows that handles mass variations and claims new results for the time-like case.
Higher-curvature EFT terms modify the photon sphere radius, critical impact parameter, and strong deflection coefficients, providing sensitive probes for constraints on quantum gravity effects via lensing and QNM spectra.
Derives EFT corrections to deflection angle, photon sphere radius, critical impact parameter, and strong lensing coefficients for Reissner-Nordström black holes in weak and strong deflection regimes.
Within two QCD-inspired equations of state coupled to Eddington-Finkelstein collapse, finite chemical potential reshapes thermodynamics but does not produce self-regularizing black hole cores.
Perturbative f(R,G) corrections shift the photon-sphere radius and shadow size, with the Gauss-Bonnet term dominating over mixed curvature contributions.
Derives the far-field light deflection angle for the Kerr-Sen black hole by constructing a refractive index that includes frame-dragging and compares the result to Kerr and Schwarzschild cases in general relativity.
Extends intrinsic curvature criteria for massive particle surfaces to stationary spacetimes and demonstrates application to black hole shadows in Kerr-family and Einstein-Maxwell-dilaton solutions.
A scalar-NED coupled black hole metric is reconstructed from an effective geometry, yielding EHT bounds on magnetic charge, Hawking-Page transition, and topological equivalence to the Reissner-Nordström solution.
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Regular black hole solutions and the quark chemical potential at the QCD phase transition
Within two QCD-inspired equations of state coupled to Eddington-Finkelstein collapse, finite chemical potential reshapes thermodynamics but does not produce self-regularizing black hole cores.