Regular black holes in quasi-topological gravity lack null thin shells in standard distributional theory, invalidating the usual mass inflation derivation and leaving inner horizon stability unresolved.
Carballo-Rubio, F
7 Pith papers cite this work. Polarity classification is still indexing.
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abstract
Mass inflation is a well established instability, conventionally associated to Cauchy horizons (which are also inner trapping horizons) of stationary geometries, leading to a divergent exponential buildup of energy. We show here that finite (but often large) exponential buildups of energy are generically present for dynamical geometries endowed with slowly-evolving inner trapping horizons, even in the absence of Cauchy horizons. This provides a more general definition of mass inflation based on quasi-local concepts. We also show that various known results in the literature are recovered in the limit in which the inner trapping horizon asymptotically approaches a Cauchy horizon. Our results imply that black hole geometries with non-extremal inner horizons, including the Kerr geometry in general relativity, and non-extremal regular black holes in theories beyond general relativity, can describe dynamical transients but not the long-lived endpoint of gravitational collapse.
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background 3representative citing papers
Surface-gravity waves in shallow water can be configured with central and graded drainage to analogize regular black holes and mimickers, enabling lab study of their instabilities.
Regular Vaidya solutions exist in effective gravitational theories that dynamically describe radiation-driven formation of regular black holes or mimickers without curvature singularities.
Charged Bardeen and Hayward metrics become singular under deformed Einstein–Maxwell equations; more stringent regularity conditions are derived and improved regular charged metrics are constructed.
Black holes with infinitely degenerate horizons are proposed to be stable against Aretakis instability, potentially serving as end states.
A spherically symmetric charged black hole evaporating via Hawking radiation can remain regular, with neither a singularity nor a Cauchy horizon, due to electromagnetic repulsion and energy-condition violation.
A regular black hole metric is constructed with sub-Planckian curvature controlled by the inner horizon radius and power-law rather than exponential mass inflation near the inner horizon.
citing papers explorer
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On mass inflation and thin shells in quasi-topological gravity
Regular black holes in quasi-topological gravity lack null thin shells in standard distributional theory, invalidating the usual mass inflation derivation and leaving inner horizon stability unresolved.
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Analog regular black holes and black hole mimickers for surface-gravity waves in fluids
Surface-gravity waves in shallow water can be configured with central and graded drainage to analogize regular black holes and mimickers, enabling lab study of their instabilities.
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Regular Vaidya solutions of effective gravitational theories
Regular Vaidya solutions exist in effective gravitational theories that dynamically describe radiation-driven formation of regular black holes or mimickers without curvature singularities.
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Charging up regular black holes
Charged Bardeen and Hayward metrics become singular under deformed Einstein–Maxwell equations; more stringent regularity conditions are derived and improved regular charged metrics are constructed.
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Taming the Aretakis instability: extremal black holes with multi-degenerate horizons
Black holes with infinitely degenerate horizons are proposed to be stable against Aretakis instability, potentially serving as end states.
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Radiating black holes in general relativity need not be singular
A spherically symmetric charged black hole evaporating via Hawking radiation can remain regular, with neither a singularity nor a Cauchy horizon, due to electromagnetic repulsion and energy-condition violation.
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Regular black hole with sub-Planckian curvature and suppressed exponential mass inflation
A regular black hole metric is constructed with sub-Planckian curvature controlled by the inner horizon radius and power-law rather than exponential mass inflation near the inner horizon.