A novel model for the problem of Quantum Gravity. The formal topologies of continuous General Relativity and discrete Quantum Mechanics are fundamentally irreconcilable without an intervening boundary constraint. We propose the dual-manifold formalism: a deterministic framework that reclassifies wave-function collapse as a localised thermodynamic phase transition. By strictly bounding quantum state reduction at the Bekenstein limit, we demonstrate that macroscopic spacetime curvature emerges natively as the mandatory metric deformation tethered to localised mass-energy. Mapped via standard thermodynamic equations of state, this localised thermal flux mechanically recovers continuous gravity without invoking unobserved dimensions or novel gauge bosons.A novel model for the problem of Quantum Gravity. The formal topologies of continuous General Relativity and discrete Quantum Mechanics are fundamentally irreconcilable without an intervening boundary constraint. We propose the dual-manifold formalism: a deterministic framework that reclassifies wave-function collapse as a localised thermodynamic phase transition. By strictly bounding quantum state reduction at the Bekenstein limit, we demonstrate that macroscopic spacetime curvature emerges natively as the mandatory metric deformation tethered to localised mass-energy. Mapped via standard thermodynamic equations of state, this localised thermal flux mechanically recovers continuous gravity without invoking unobserved dimensions or novel gauge bosons.

Aug 26, 20260 citations

Two approaches to measurability conception and quantum theory

Alexander Shalyt-Margolin

Advanced Studies in Theoretical PhysicsJan 1, 20171 citation

Generalized entanglement temperature and entanglement thermodynamics

Ashis Saha, Sunandan Gangopadhyay, Jyoti Prasad Saha

In this paper, we observe that a Smarr like thermodynamic relation is satisfied by the HEE of a gravity background dual to a nonconformal field theory. Such a relation emerges naturally by demanding that the generalized entanglement temperature ( $T_g$ ) produces the exact Hawking temperature as the leading term in the IR limit ( $l\rightarrow \infty$ ). In the UV limit ( $l\rightarrow 0$ ) the leading term of the generalized entanglement temperature ( $T_g$ ) gives the entanglement temperature which is inversely proportional to the subsystem size $l$ . The results reduces to the existing results in the limiting case of the nonconformal parameter going to zero.In this paper, we observe that a Smarr like thermodynamic relation is satisfied by the HEE of a gravity background dual to a nonconformal field theory. Such a relation emerges naturally by demanding that the generalized entanglement temperature ($T_g$) produces the exact Hawking temperature as the leading term in the IR limit ($l\rightarrow \infty$). In the UV limit ($l\rightarrow 0$) the leading term of the generalized entanglement temperature ($T_g$) gives the entanglement temperature which is inversely proportional to the subsystem size $l$. The results reduces to the existing results in the limiting case of the nonconformal parameter going to zero.

Apr 2, 20200 citations

Hawking-Page phase transition for pure Lovelock black holes

Nitesh K. Dubey, Sanved Kolekar

We investigate the thermodynamic properties of static, spherically symmetric Anti-de Sitter (AdS) black holes, focusing on the interplay between characteristic temperatures, as well as on the universality of Ruppeiner scalar curvature at the Hawking-Page (HP) phase transition. In particular, we study the relation between the minimum temperature and the HP phase transition temperature for static, spherically symmetric AdS black holes in pure Lovelock gravity. For the electromagnetically neutral case in Einstein gravity, the minimum temperature in $(d+1)$ dimensions coincides with the HP transition temperature in $d$ dimensions, while in higher pure Lovelock theories this relation is modified by a dimension- and order-dependent factor, reducing to the Einstein result in appropriate limits. For charged AdS black holes, in the grand canonical ensemble, in general relativity, the two temperatures differ by a simple dimension-dependent factor, whereas no universal relation persists in higher curvature pure Lovelock theories. We further analyze the normalized Ruppeiner scalar curvature at the HP transition and show that it is a universal constant depending only on the spacetime dimension for electromagnetically neutral black holes in pure Lovelock theories. The normalized scalar curvature remains a constant, under appropriate conditions, even for the charged static spherically symmetric black holes in the grand canonical ensemble for the Einstein theory case, whereas in general pure Lovelock theories it depends on thermodynamic parameters such as pressure and electrostatic potential, asymptotically approaching a constant in the large-pressure or simultaneous large-potential and large-pressure limits.We investigate the thermodynamic properties of static, spherically symmetric Anti-de Sitter (AdS) black holes, focusing on the interplay between characteristic temperatures, as well as on the universality of Ruppeiner scalar curvature at the Hawking-Page (HP) phase transition. In particular, we study the relation between the minimum temperature and the HP phase transition temperature for static, spherically symmetric AdS black holes in pure Lovelock gravity. For the electromagnetically neutral case in Einstein gravity, the minimum temperature in $(d+1)$ dimensions coincides with the HP transition temperature in $d$ dimensions, while in higher pure Lovelock theories this relation is modified by a dimension- and order-dependent factor, reducing to the Einstein result in appropriate limits. For charged AdS black holes, in the grand canonical ensemble, in general relativity, the two temperatures differ by a simple dimension-dependent factor, whereas no universal relation persists in higher curvature pure Lovelock theories. We further analyze the normalized Ruppeiner scalar curvature at the HP transition and show that it is a universal constant depending only on the spacetime dimension for electromagnetically neutral black holes in pure Lovelock theories. The normalized scalar curvature remains a constant, under appropriate conditions, even for the charged static spherically symmetric black holes in the grand canonical ensemble for the Einstein theory case, whereas in general pure Lovelock theories it depends on thermodynamic parameters such as pressure and electrostatic potential, asymptotically approaching a constant in the large-pressure or simultaneous large-potential and large-pressure limits.

gr-qcCross-listedarXiv:2606.10647Jun 10, 2026

Simultaneous measurability in quantum theory

James L Park, Henry Margenau

International Journal of Theoretical PhysicsOct 1, 1968127 citations

Entanglement Islands and Thermodynamics of the Black Hole in Asymptotically Safe Quantum Gravity

Sobhan Kazempour, Sichun Sun, Chengye Yu

We study thermodynamic properties and the entanglement island of a black hole in asymptotically safe quantum gravity, analyzing key thermodynamic quantities such as the Hawking temperature, heat capacity, and entropy, as well as the mass-horizon radius relation. Unlike Schwarzschild black holes, the temperature decreases with mass near the evaporation endpoint, signaling a phase transition and possible stable remnant. The entanglement entropy of Hawking radiation is obtained both with and without island contributions. Without islands, the radiation entropy grows linearly indefinitely, leading to the information paradox. By including island contributions and extremizing the generalized entropy functional, we resolve this paradox. At late times, the radiation entropy saturates at the Bekenstein-Hawking entropy, confirming unitary evolution. From this, we derive the Page time and scrambling time by equating early- and late-time entanglement entropies. The result of this study establishes the finiteness of the radiation entropy and consistency with quantum mechanics.We study thermodynamic properties and the entanglement island of a black hole in asymptotically safe quantum gravity, analyzing key thermodynamic quantities such as the Hawking temperature, heat capacity, and entropy, as well as the mass-horizon radius relation. Unlike Schwarzschild black holes, the temperature decreases with mass near the evaporation endpoint, signaling a phase transition and possible stable remnant. The entanglement entropy of Hawking radiation is obtained both with and without island contributions. Without islands, the radiation entropy grows linearly indefinitely, leading to the information paradox. By including island contributions and extremizing the generalized entropy functional, we resolve this paradox. At late times, the radiation entropy saturates at the Bekenstein-Hawking entropy, confirming unitary evolution. From this, we derive the Page time and scrambling time by equating early- and late-time entanglement entropies. The result of this study establishes the finiteness of the radiation entropy and consistency with quantum mechanics.

gr-qcCross-listedarXiv:2512.21995Dec 29, 2025

T_g

) produces the exact Hawking temperature as the leading term in the IR limit (

l\rightarrow \infty

). In the UV limit (

l\rightarrow 0

) the leading term of the generalized entanglement temperature (

T_g

) gives the entanglement temperature which is inversely proportional to the subsystem size

l

. The results reduces to the existing results in the limiting case of the nonconformal parameter going to zero.

(d+1)

dimensions coincides with the HP transition temperature in

d

dimensions, while in higher pure Lovelock theories this relation is modified by a dimension- and order-dependent factor, reducing to the Einstein result in appropriate limits. For charged AdS black holes, in the grand canonical ensemble, in general relativity, the two temperatures differ by a simple dimension-dependent factor, whereas no universal relation persists in higher curvature pure Lovelock theories. We further analyze the normalized Ruppeiner scalar curvature at the HP transition and show that it is a universal constant depending only on the spacetime dimension for electromagnetically neutral black holes in pure Lovelock theories. The normalized scalar curvature remains a constant, under appropriate conditions, even for the charged static spherically symmetric black holes in the grand canonical ensemble for the Einstein theory case, whereas in general pure Lovelock theories it depends on thermodynamic parameters such as pressure and electrostatic potential, asymptotically approaching a constant in the large-pressure or simultaneous large-potential and large-pressure limits.