REVIEW 7 cited by
Holographic explorations of regular black holes in pure gravity
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
Holographic explorations of regular black holes in pure gravity
read the original abstract
It has been recently established in \textit{Phys.Lett.B 861 (2025) 139260} that regular, asymptotically flat black holes exist in pure gravity theories in dimension greater than four. We extend this result to asymptotically Anti-de Sitter spacetimes and perform bottom-up holographic explorations: Hawking-Page phase transitions, quasinormal modes of black holes providing decay times of excitations in the finite temperature conformal field theory and U-shaped string probes leading to the quark-antiquark potential in the dual field theory. The gravitational action contains a bared, negative cosmological constant and an Einstein-Hilbert term, supplemented by an infinite series of higher-curvature terms of the family known as Quasi-topological (QT) Lagrangians, leading to a lapse function in terms of infinite series which can be resumed to an analytic function for different coupling choices. The QT terms are defined as those satisfying a Birkhoff's theorem and possessing a holographic c-function, and exist at all orders in the curvature, for arbitrary dimension greater than four. Besides presenting the general formulae, we explore the physics of three specific cases leading to Hayward, Dymnikova and Bardeen-like regular black holes. We also found the field redefinition that permits recasting the $\alpha'^3 W^4$ correction of Type IIB supergravity on $\mathcal{A}_5\times S^5$ as a series of QT terms. Before finishing, beyond holography, we also provide an extended thermodynamic setup, that via variations of the dimensionful $\alpha$ and $L$, allow obtaining the Euler relation between finite thermodynamical quantities for the black hole of the theory.
Forward citations
Cited by 7 Pith papers
-
Regular Black Holes in Nonlocal Quasitopological Gravity
Infinite-derivative completions of quasitopological gravities are ghost-free, avoid strong coupling, and admit exact spherically symmetric vacuum regular black holes obeying a perturbative Birkhoff theorem.
-
Cosmic Inflation From Regular Black Holes
Regular black holes in the bulk of quasi-topological gravity drive a de Sitter inflationary phase on the brane at small scales, with e-fold number set by the ratio of black hole radius to higher-curvature scale.
-
All $2D$ generalised dilaton theories from $d\geq 4$ gravities
Generic 2D Horndeski theories arise from dimensional reduction of d≥4 gravities, yielding a Birkhoff theorem for quasi-topological gravities where static spherically symmetric solutions satisfy g_tt g_rr = -1 and are ...
-
Null geodesic defocusing in dynamical black-hole-to-white-hole transitions
Dynamical black-hole-to-white-hole transitions require a violation of the null convergence condition for the trapped region to disappear and the anti-trapped region to form.
-
$g_{tt}g_{rr} =-1$ black hole thermodynamics in extended quasi-topological gravity
A unified framework links the generating function for static black holes satisfying g_tt g_rr=-1 in extended quasi-topological gravity to thermodynamic mass and Wald entropy via an effective 2D dilaton theory.
-
$O(d,d)$ symmetric gravity and finite coupling holography
In O(d,d) symmetric gravity with curvature corrections, black brane singularities persist with altered Kasner exponents, while dilaton effects enable dynamic generation of negative cosmological constants at weak coupling.
-
$O(d,d)$ symmetric gravity and finite coupling holography
In O(d,d) symmetric gravity with curvature corrections, black brane singularities are not resolved but approach with altered Kasner exponents, while a dilaton generates negative cosmological constants at small coupling.
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.