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Exact Regular Black Hole Solutions with de Sitter Cores and Hagedorn Fluid
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Exact Regular Black Hole Solutions with de Sitter Cores and Hagedorn Fluid
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In this paper, we present three exact solutions to the Einstein field equations, each illustrating different black hole models. The first solution introduces a black hole with a variable equation of state, $P = k(r)\rho$, which can represent both singular and regular black holes depending on the parameters $M_0$ and $w_0$. The second solution features a black hole with Hagedorn fluid, relevant to the late stages of black hole formation, and reveals similarities to the first solution by also describing both singular and regular black holes in a specific case. Furthermore, we investigate the shadows cast by these black hole solutions to constrain their parameters. Recognizing that real astrophysical black holes are dynamic, we developed a third, dynamical solution that addresses gravitational collapse and suggests the potential formation of naked singularities. This indicates that a black hole can transition from regular to singular and back to regular during its evolution.
Forward citations
Cited by 7 Pith papers
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The formation of a regular black hole could release gamma-ray-burst-scale energy only if its singularity-avoiding core is a weak perturbation of Schwarzschild.
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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.
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A de Sitter-core black hole with parameters M0 and R exhibits lowered quasinormal frequencies, stronger greybody suppression, reduced Hawking temperature, and a mildly smaller shadow relative to Schwarzschild.
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