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.
Huang and X.-P
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abstract
Regular black holes without curvature singularity can arise in Einstein gravity with appropriate matter energy-momentum tensor. We show that these regular solutions represent only a special case of a much broader family of black holes with a free mass parameter. The regularity is achieved only at a specific mass value, and any deviation from the fine-tuned parameter inevitably results in curvature singularity. As a concrete example, we consider nonlinear electrodynamics (NLED) as matter sources. A new NLED theory is proposed that is a generalization of the Bardeen class and the Hayward class. New regular black holes and their singular counterparts are obtained. Significant distinctions between regular black holes and their singular counterparts are analyzed. These findings provide new insights into regular black holes.
representative citing papers
Lorentzian-Euclidean black holes produce excess inner-shadow intensity and accumulate energy at the horizon with backreaction unlike stable light rings.
Regular primordial black holes can evaporate completely like singular ones and yield the observed dark matter density under modified cosmological constraints.
citing papers explorer
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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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Shadow signatures and energy accumulation in Lorentzian-Euclidean black holes
Lorentzian-Euclidean black holes produce excess inner-shadow intensity and accumulate energy at the horizon with backreaction unlike stable light rings.
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Dark matter production from evaporation of regular primordial black holes
Regular primordial black holes can evaporate completely like singular ones and yield the observed dark matter density under modified cosmological constraints.