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Hairy Black Holes from Horndeski Theory

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arxiv 2107.07839 v2 pith:HLWHAGZ4 submitted 2021-07-16 gr-qc

Santiago Esteban Perez Bergliaffa , Rodrigo Maier , Nathan de Oliveira Silvano This is my paper
classification gr-qc
keywords blackholehorizonsolutionconstantscorrectioncouplingdomain
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abstract

We present an exact static black hole solution of Einstein field equations in the framework of Horndeski Theory by imposing spherical symmetry and choosing the coupling constants in the Lagrangian so that the only singularity in the solution is at $r=0$. The analytical extension is built in two particular domains of the parametric space. In the first domain we obtain a solution exhibiting an event horizon analogous to that of the Schwarzschild geometry. For the second domain, we show that the metric displays an exterior event horizon and a Cauchy horizon which encloses a singularity. For both branches we obtain the corresponding Hawking temperature which, when compared to that of the Schwarzschild black hole, acquires a correction proportional to a combination of the coupling constants. Such a correction also modifies the definition of the entropy of the black hole.

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Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Energy conditions in static, spherically symmetric spacetimes and effective geometries

    gr-qc 2026-04 unverdicted novelty 5.0 of 10

    A logarithmic correction to Schwarzschild in static spherical symmetry obeys all classical energy conditions and serves as an effective exterior for horizon-bearing and horizonless compact objects.

  2. Energy conditions in static, spherically symmetric spacetimes and effective geometries

    gr-qc 2026-04 unverdicted novelty 5.0 of 10

    A constructive algorithm yields NEC-obeying static spherical metrics with g_tt g_rr = -1, including a log-corrected Schwarzschild geometry that can mimic black holes.

  3. Probing Horndeski Gravity via Kerr Black Hole: Insights from Thin Accretion Disks and Shadows with EHT Observations

    gr-qc 2025-09 conditional novelty 5.0 of 10

    For a rotating Horndeski black hole, the hair parameter h shrinks and deforms the shadow, and EHT shadow sizes allow but do not uniquely confirm a non-zero h.

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