# On relativistic generalization of Perelman’s W-entropy and thermodynamic description of gravitational fields and cosmology

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## Abstract

Using double \(2+2\) and \(3+1\) nonholonomic fibrations on Lorentz manifolds, we extend the concept of W-entropy for gravitational fields in general relativity (GR). Such F- and W-functionals were introduced in the Ricci flow theory of three dimensional (3-d) Riemannian metrics by Perelman (the entropy formula for the Ricci flow and its geometric applications. arXiv:math.DG/0211159). Non-relativistic 3-d Ricci flows are characterized by associated statistical thermodynamical values determined by W-entropy. Generalizations for geometric flows of 4-d pseudo-Riemannian metrics are considered for models with local thermodynamical equilibrium and separation of dissipative and non-dissipative processes in relativistic hydrodynamics. The approach is elaborated in the framework of classical field theories (relativistic continuum and hydrodynamic models) without an underlying kinetic description, which will be elaborated in other work. The \(3+1\) splitting allows us to provide a general relativistic definition of gravitational entropy in the Lyapunov–Perelman sense. It increases monotonically as structure forms in the Universe. We can formulate a thermodynamic description of exact solutions in GR depending, in general, on all spacetime coordinates. A corresponding \(2+2\) splitting with nonholonomic deformation of linear connection and frame structures is necessary for generating in very general form various classes of exact solutions of the Einstein and general relativistic geometric flow equations. Finally, we speculate on physical macrostates and microstate interpretations of the W-entropy in GR, geometric flow theories and possible connections to string theory (a second unsolved problem also contained in Perelman’s work) in Polyakov’s approach.

## 1 Introduction

Perelman defined the W-entropy [1, 2, 3] as a functional with a non-decreasing Lyapunov-type property from which Hamilton’s equations [4, 5, 6] for Ricci flows can be derived following the variational procedure. The approach was elaborated upon for the geometric evolution of three dimensional (3-d) Riemannian metrics. There were obtained a number of fundamental results in geometric analysis and topology. Such directions in modern mathematics became famous after the elaborated methods allowed one to prove the Poincaré and Thorston conjectures. In this paper we show that using nonholonomic double \(3+1\) and \(2+2\) splitting in general relativity (GR) the geometric and statistical thermodynamics methods considered in Perelman’s work can be developed for theories of generalized relativistic geometric flows. We consider how such constructions can be applied in modern cosmology and astrophysics.

There are different ways for generalizing models of 3-d Ricci flow evolution for 4-d spacetimes with pseudo-Euclidean signature. For instance, there were formulated theories of stochastic/diffusion and kinetic processes with local anisotropy, fractional geometric evolution etc [7, 8, 9]. It is possible to construct thermo field models of Ricci flow evolution on imaginary time \(\varsigma =-\mathrm{{it}}(0\le \varsigma \le 1/\kappa T,\) where \(\kappa \) is Boltzmann’s constant and *T* is the temperature). In such a case, the pseudo-Riemannian spacetime is transformed into a Riemannian configuration space-like in thermal and/or finite temperature quantum field theory (see [10, 11] and the references therein). Here we recall that Perelman treated \(\tau =\varsigma ^{-1}\) as a temperature parameter and derived his W-entropy by analogy to formulas for the entropy in statistical mechanics.^{1} In his work, it was not specified what type of underlying microstates and their energy should be taken in order to explain the geometric flows corresponding to certain thermodynamical and gravity models.

Geometric flow evolution models of pseudo-Riemannian metrics have not been formulated and studied in modern physical mathematics. Such ideas have not been developed and do not exist among gravitational and related relativistic thermodynamics/diffusion/kinetic theories. In quantum field theory some examples were considered in relativistic form of low dimensional geometric flow equations of type (1). That was even before mathematicians formulated in rigorous form respective directions in geometric analysis and topology which are related to the Ricci flow theory. Friedan published during 1980–1985 a series of works on nonlinear sigma models, \(\sigma \)-models, in two \(+\) epsilon dimensions; see [15, 16, 17]. Certain topological properties were studied of the \(\beta \) function and solutions of the fixed-point equation (the latter called the Ricci soliton equation) and further developments on renormalization of the \( O (N)\)-invariant nonlinear \(\sigma \)-models in the low-temperature regime dominated by small fluctuations around ordered states [18].

Generalized Perelman’s functionals were studied for various models of non-Riemannian geometries and (modified) gravity theories; see [19, 21, 22] and the references therein. The corresponding generalized Ricci soliton equations describe modified Einstein equations for certain classes of modified gravity theories, MGTs. Such models possess an important decoupling property of the fundamental evolution/dynamical equations and can be integrated in general form. We can study new classes of exact solutions and search for application in modern gravity and cosmology. Nevertheless, we cannot argue that certain analogs of generalized/modified Hamilton’s equations would describe in a self-consistent manner certain evolution processes if additional assumptions on geometric and physical properties of GR flows are not considered. We cannot treat any formal relativistic modification of Perelman’s functionals defined only in terms of the Levi-Civita connection for pseudo-Riemannian metrics as an entropy functional. For the geometric flow evolution of 4-d metrics with Lorentz signature and non-stationary solutions in GR, it is not possible to formulate a statistical thermodynamic interpretation like in the case of 3-d Riemannian ones.

The main goal of this paper is to study how the concept of W-entropy can be generalized in order to characterize 3-d hypersurface gravitational thermodynamic configurations and their GR evolution determined by exact solutions in Einstein gravity. The approach involves two other less established (general) relativistic theories: the relativistic statistical thermodynamics and the nonlinear diffusion theory on curved spacetimes and in gravity. Historically, the first relativistic generalizations of thermodynamics due to Planck [23] and Einstein [24] were subject to certain criticisms and modifications more than half century later [25, 26, 27, 28, 29, 30, 31]. Various ideas and constructions exclude each other and various debates continue even today [32, 33, 34, 35, 36, 37, 38]. For such models, different covariant relativistic thermodynamical and/or statistical thermodynamical values were postulated, with respective transformation laws under local Lorentz transforms. There is an explicit dependence on the fourth time-like coordinate and the main issue is how to define the concept of temperature and provide a physical interpretation. We plan to elaborate on a general thermodynamic treatment of relativistic Ricci flows using methods of relativistic kinetics and nonlinear diffusion theory in our further work. In this paper, we consider a generalization of Perelman’s W-thermodynamic model to flows of entropy and effective energy in the framework of “most simple” relativistic fluids theory and hydrodynamics with stability and causality.

The relativistic 4-d geometric flows depend, in general, on a time-like coordinate being described also by evolution on a temperature-like parameter. We argue that an appropriate redefinition of effective thermodynamic variables for the Ricci flow theory allows us to compute the entropy of gravitational fields and elaborate upon an effective statistical mechanics and thermodynamical formalism both for cosmology and black holes. We shall use the \(3+1\) decomposition formalism (see [39] and the references therein) and specify the conditions when a 3-d geometric evolution is “driven” in relativistic form by solutions of the Einstein equations in GR. Vacuum stationary solutions with Killing symmetries and horizons consist of a special class of gravitational configurations when the thermodynamic models are constructed for the entropy determined by the horizon gravity for a corresponding \(2+1+1\) splitting.

We compare our relativistic geometric flow approach to a recently proposed thermodynamical theory of gravitational fields with a measure of gravitational entropy was proposed in Ref. [40] (the so-called CET model). Those constructions are based on the square-root of the Bel–Robinson tensor when the measure is non-negative in contrast to other proposals. There were analyzed some examples, for instance, for the Schwarzschild black hole and Friedmann–Lemaître–Robertson–Worker, FLRW, cosmology. The black hole thermodynamics was derived as a particular case for stationary spacetimes. We study how the CET model can be obtained by corresponding nonholonomic parameterizations from the statistical mechanics and thermodynamic models based on the concept of W-entropy (see further developments in [19, 20, 21, 22] and the references therein). There is not a unique way to generalize standard black hole thermodynamical constructions in order to include cosmological solutions. A geometric self-consistent variant is to address such problems using relativistic models with generalized W-entropy. In this work, we prove that there are such nonholonomic double \(3+1\) and \(2+2\) splitting when a relativistic generalization of statistical thermodynamics of geometric flows is possible for general classes of cosmological and other type solutions.

A definition of gravitational entropy which would be compatible with time depending and structure formation cosmological processes needs to be valid for very general classes of solutions with non-stationary and/or non-vacuum spacetimes. In order to prove that our approach really provides such a possibility, we shall apply the so-called anholonomic frame deformation method, AFDM (see a recent review in [41] and the references therein) for constructing generic off-diagonal exact solutions in various models of gravity theories and geometric flows with commutative and noncommutative variables [19, 21, 42]. This method involves \(2+2\) nonholonomic fibrations and a geometric techniques which allows us to integrate systems of partial differential equations (PDEs) with functional and parametric dependencies on generating and integration functions and constants depending, in general, on all spacetime coordinates and with various types of Killing and non-Killing symmetries.

The article is organized as follows: in Sect. 2, we provide an introduction into the geometry of double nonholonomic \(3+1\) and \(2+2\) fibrations of Lorentz manifolds. The main geometric and physical objects and the Einstein equations are written in nonholonomic variables adapted to a general double splitting.

Section 3 is devoted to the theory of relativistic Ricci flows with nonholonomic constraints for \(3+1\) splitting and auxiliary connections completely defined by the metric and nonlinear connection structures. The geometric evolution of the Levi-Civita configurations (with zero nonholonomically induced torsion) is considered as a special case defined by nonholonomic constraints. There are considered generalizations of Perelman’s functionals on Lorentz manifolds and derived the equations for the geometric relativistic evolution.

Section 4 is a summary of the anholonomic frame deformation method (AFDM) of constructing generic off-diagonal solutions in GR. Examples are considered of inhomogeneous and locally anisotropic cosmological solutions and black hole/ellipsoid solutions with self-consistent off-diagonal deformations and solitonic interactions.

In Sect. 5, a model of statistical thermodynamics is elaborated for gravitational 3-d hypersurface configurations and with relativistic evolution on (associated) Einstein manifolds. We show how to compute Perelman’s thermodynamical values for explicit examples of generic off-diagonal solutions in GR. It is analyzed how the relativistic W-entropy thermodynamics can be parameterized in order to model the CET thermodynamics and standard black hole physics. A general relativistic thermodynamic model for geometric flows of exact solutions in GR is elaborated following ideas and methods of relativistic hydrodynamics. Final remarks and conclusions are presented in Sect. 6.

## 2 Double \(2+2\) and \(3+1\) nonholonomic fibrations in GR

We provide an introduction into the geometry double \(2+2\) and \(3+1\) fibrations of Lorentz spacetime manifolds defined as follows in this section. The \(2+2\) splitting with nonholonomic deformations of the local frame and linear connection structures allowed one to decouple the Einstein equations in general form and to construct exact solutions with generic off-diagonal metrics depending on all space coordinates. Such nonholonomic \(2+2\) methods were applied for deformation and A-brane quantization of theories of gravity [19, 41, 42]. The \(3+1\) decomposition was introduced in GR with the aim to elaborate canonical approaches, for instance, to perturbative quantum gravity, relativistic thermodynamics etc. (for review of results see [39]). Working with nonholonomic distributions adapted to a conventional double \(3+1\) and \(2+2\) splitting, we can formulate an unified geometric approach to general relativistic Ricci flow and thermodynamical theories and apply the geometric methods for generating exact solutions of fundamental evolution and/or gravitational and matter fields equations.

### 2.1 Nonholonomic \(2+2\) splitting and nonlinear connections in GR

We consider a spacetime \(\, _{1}^{3}V\) in GR as a 4-d real smooth, i.e. \( \mathcal {C}^{\infty }\), Lorentz manifold \((V,\mathbf {g})\) determined by a pseudo-Riemannian metric \(\mathbf {g}\) of signature \((+,+,+,-).\) ^{2} It is assumed that it is possible to divide continuously over *V* each light cone of the metric \(\mathbf {g}\) into past and future paths. This means that \(\, _{1}^{3}V\) is time orientable. The tangent bundle of \(V_{1}^{3}\) is defined as the union of all tangent spaces \( T_{u}(\, _{1}^{3}V)\) is considered for all points \(u\in \, _{1}^{3}V,\) i.e. \( T(\, _{1}^{3}V):=\bigcup _{u}T_{u}(\, _{1}^{3}V).\) The typical fibers of \( T(\, _{1}^{3}V)\) are Minkowski spaces with pseudo-Euclidean signature. The dual bundle (equivalently, the cotangent bundle) of \(T(\, _{1}^{3}V)\) is denoted \(T^{*}(\, _{1}^{3}V).\) We shall write *TV* for the space of smooth vector fields and, respectively, \(T^{*}V\) for the space of 1-forms on a real 4-d spacetime manifold *V*, omitting left labels on signature if that will not result in ambiguities. In rigorous mathematical form, we can use the axiomatic approach to GR beginning in 1996 due to Ehlers et al. (the so-called EPS axioms) [43]; see further developments in [44, 45, 46]. In order to formulate in standard form the gravitational field equations in GR, the Einstein equations, it is used the unique metric compatible and torsionless Levi-Civita (LC) connection \(\nabla .\) The theory of GR was reformulated in various type of tetradic, spinor etc. variables and corresponding connection structures introduced with various purposes, for instance, to study solutions of the Einstein–Yang–Mills–Higgs–Dirac (EYMHD) systems [47, 48]. In so-called nonholonomic variables with an auxiliary canonical distinguished connection structure \(\widehat{\mathbf {D}}\) (see below the definition given in Eq. (9)), the EYMHD equations can be decoupled and integrated in very general forms with solutions depending, in general, on all spacetime coordinates. Fortunately, the EPS axiomatic can be generalized for spacetimes enabled with nonholonomic distributions and fibrations (for GR and various MGTs, see [49, 50, 51]). This provides a rigorous mathematical background for elaborating theories of general relativistic geometric evolution with nonholonomic variables on Lorentz manifolds, which is the main subject for study in this work.

*h*, and 2-d vertical, 2, subspaces (the local subspaces are of different signature). This defines a nonlinear connection (N-connection) structure,

*h*, and vertical,

*v*, subspaces. In our approach, boldface symbols are used in order to emphasize that certain spaces and/or geometric objects are for spaces endowed with N-connection structure. For simplicity, we shall write \(\mathbf {V}=(\, _{1}^{3}V,\mathbf {N} )\) for a Lorentz manifold with a

*h*–

*v*-decomposition (2). This is an example of a nonholonomic manifold consisting, in our case, from a pseudo-Riemannian manifold and a nonholonomic (equivalently, anholonomic, or non-integrable) distribution \(\mathbf {N.}\)

^{3}In local form, a N-connection is stated by a set of coefficients \( N_{i}^{a}(u)\) when \(\mathbf {N}=N_{i}^{a}\mathrm{d}x^{i}\otimes \partial _{a},\) where \( \partial _{a}=\partial /\partial y^{a}.\)

^{4}

On any nonholonomic spacetime \(\mathbf {V,}\) we can consider covariant derivatives determined by affine (linear) connections which are adapted to the N-connection splitting. A *distinguished connection, d-connection,* is a linear connection \(\mathbf {D}=(h\mathbf {D},v\mathbf {D} )\) which preserves under parallel transport the splitting (2). In general, a linear connection *D* is not adapted to a prescribed *h*–*v*-decomposition, i.e. it is not a d-connection (we do not use a boldface symbol for non-N-adapted connections).

*h*- and

*v*-indices,

*e*determined for the

*h*–

*v*-components of \(\mathbf {D}_{\mathbf {e}_{\alpha }}\mathbf {e}_{\beta }:= \mathbf {D} _{\alpha }\mathbf {e}_{\beta }\) using \(\mathbf {X}=\mathbf {e}_{\alpha }\) and \( \mathbf {Y}=\mathbf {e}_{\beta }.\)

*h*- and

*v*-subspaces. We note that there are non-zero torsion components, \(hv\widehat{\mathcal {T}},\) with non-zero mixed indices with respect to a N-adapted basis (3) and/or (4). Nevertheless, this torsion field \(\widehat{\mathcal {T}}\) is completely defined by the metric field following the parameterization (8) with \((h\mathbf {g},v\mathbf {g;N}).\)

The Ricci tensors of \(\widehat{\mathbf {D}}\) and \(\nabla \) are defined and computed in the standard way and denoted, respectively, by \(\ \widehat{ \mathcal {R}}ic=\{\widehat{\mathbf {R}}_{\ \beta \gamma }:=\widehat{\mathbf {R}} _{\ \alpha \beta \gamma }^{\gamma }\}\) and \(Ric=\{R_{\ \beta \gamma }:=R_{\ \alpha \beta \gamma }^{\gamma }\}.\) The N-adapted coefficients for \( \widehat{\mathbf {D}}\) and the corresponding torsion, \(\widehat{\mathbf {T}}_{\ \alpha \beta }^{\gamma },\) Ricci d-tensor, \(\widehat{\mathbf {R}}_{\ \beta \gamma },\) and Einstein d-tensor, \(\widehat{\mathbf {E}}_{\ \beta \gamma },\) are computed in [41, 42]. Any (pseudo) Riemannian geometry can be equivalently described by both geometric data \(( \mathbf {g,}\varvec{\nabla } ) \) and \((\mathbf {g,N,}\widehat{\mathbf {D}}),\) when the canonical distortion relations \(\widehat{\mathcal {R}}=\ ^{\nabla }\mathcal {R+}\ ^{\nabla }\mathcal {Z}\) and \(\widehat{\mathcal {R}}ic=Ric+\widehat{\mathcal {Z}} ic,\) with respective distortion d-tensors \(\ ^{\nabla }\mathcal {Z}\) and \( \widehat{\mathcal {Z}}ic,\) are computed for the canonical distortion relations \(\widehat{\mathbf {D}}=\nabla +\widehat{\mathbf {Z}}.\)

*h*-

*v*N-adapted coefficients,

*R*; they are taken for the Levi-Civita connection \(\nabla \) of \(g_{\alpha \beta }.\) In these formulas, \(\ ^{m}T_{\alpha \beta }\) is the energy-momentum tensor of matter fields \(\ ^{A}\varphi \) determined by a general Lagrangian \(\ ^{m}\mathcal {L} (\mathbf {g,}\nabla ,\ \ ^{A}\varphi )\) and \(\varkappa \) is the gravitational coupling constant for GR.

^{5}The gravitational field equations in GR can be rewritten equivalently using the canonical d-connection [41, 42],

^{6}We can integrate nonholonomic deformations of the Einstein equations in very general form and construct exact solutions parameterized by generic off-diagonal metrics depending on all spacetime coordinates via the respective classes of generating functions and integration functions and constants. Having constructed certain general classes of solutions, we can impose at the end the LC-conditions (14) and extract LC-configurations \(\widehat{\mathbf {D}}_{\mid \widehat{\mathcal {T}}=0}=\nabla .\) This allows one, for instance, to construct new classes of generic off-diagonal solutions of (12) in GR and various MGTs. We note that to find nontrivial off-diagonal solutions is important to impose the LC-conditions (14) after a class of solutions of (13) for \(\widehat{\mathbf {D}}\) are constructed in general form. If we work only with \(\nabla ,\) we are not able to decouple the Einstein equations in general form.

### 2.2 \(3+1\) Decompositions adapted to nonholonomic \(2+2\) splitting

We foliate a 4-d Lorentzian nonholonomic manifold \(\mathbf {V}=(\, _{1}^{3}V, \mathbf {N})\) enabled with a pseudo-Riemannian metric \(\mathbf {g} =\{g_{\alpha \beta }\}\) of signature \((+++-)\) into a family of non-intersecting space-like 3-d hypersurfaces \(\Xi _{t}\) parameterized by a scalar field, i.e. the “time function”, \(t(u^{\alpha }),\) as described as follows. Such a \(3+1\) spacetime decomposition is necessary for elaborating various thermodynamic and flow models when a conventional splitting into time- and space-like coordinates is important for definition of physical important values (like entropy, effective energy etc.) and fundamental geometric evolution equations. We have to generalize the well-known geometric \(3+1\) formalism [39] to the case of spacetimes enabled with the nontrivial N-connection structure [41, 42].

A hypersurface \(\Xi \subset \mathbf {V}\) is considered as an one-to-one image of a 3-d manifold \({\,}_{\shortmid }\Xi .\) This image is given by an embedding \(\Xi =\zeta (\, _{\shortmid }\Xi )\) constructed as an homeomorphism with both continuous maps \(\zeta \) and \(\zeta ^{-1}.\) This guarantees that \( \Xi \) does not intersect itself. We shall use a left “up” or “low” label by a vertical bar “\(\, _{\shortmid }\ \)” in order to emphasize that a manifold is 3-d, or certain geometric objects refer to 3-d manifolds/hypersurfaces. Locally, a hypersurface is considered as the set of points for which a scalar field *t* on \(\mathbf {V}\) is constant, for instance, i.e. \(t(p)=0,\forall \) \(p\in \Xi .\) We assume that *t* spans \(\mathbb {R}\) and \( \Xi \) is a connected submanifold of \(\mathbf {V}\) with topology \(\mathbb {R} ^{3}.\) The local coordinates for a \(3+1\) splitting are labeled \(u^{\alpha }=(x^{\grave{\imath }},t),\) where the indices \(\alpha ,\beta ,\ldots =1,2,3,4\) and \( \grave{\imath },\grave{j},\ldots =1,2,3.\) In brief, we shall write \(u=(\breve{u} ,t).\) The mapping \(\zeta \) “carries along” curves/vectors in \(\, _{\shortmid }\Xi \) to curves/vectors in \(\mathbf {V,}\) for \(\zeta :(x^{\grave{\imath } })\longrightarrow (x^{\grave{\imath }},0).\) This defines respective local bases \(\partial _{\grave{\imath }}:=\partial /\partial x^{\grave{\imath }}\in T {(\, _{\shortmid }\varvec{\Xi } )}\) and \(\partial _{\alpha }:=\partial /\partial u^{\alpha }\in T\mathbf {V.}\) Correspondingly, the coefficients of 3-vectors and 4-vectors are expressed \(\, _{\shortmid }\mathbf {a}=a^{\grave{ \imath }}\partial _{\grave{\imath }}\) and \(\,\mathbf {a}=a^{\alpha }\partial _{\alpha }\) (for convenience, we shall use also capital letters, for instance, \(\, _{\shortmid }\mathbf {A}=A^{\grave{\imath }}\partial _{ \grave{\imath }}\) and \(\mathbf {\ A}=A^{\alpha }\partial _{\alpha }).\) For dual forms to vectors, 1-forms, we use the respective dual bases \(\mathbf {d}x^{ \grave{\imath }}\in T^{*}{(\, _{\shortmid }\varvec{\Xi } )}\) and \( \mathrm{d}u^{\alpha }\in T^{*}\mathbf {V.}\) We shall write for 1-forms \(\, _{\shortmid }{\tilde{\mathbf {A}}}=A_{\grave{\imath }}\mathbf {d}x^{\grave{\imath } }\) and \({\tilde{\mathbf {A}}}=A_{\alpha }\mathrm{d}u^{\alpha }\) and omit the left/up label by a tilde \({\sim } \) (writing \(\, _{\shortmid }\mathbf {A}\) and \( \mathbf {A)}\) if that will not result in ambiguities.

#### 2.2.1 Induced N-adapted 3-d hypersurface metrics

*t*as a parameter for a congruence of curves \(\chi (t)\subset \, _{1}^{3}V\) intersecting \(\Sigma _{t},\) when the vector \(\mathbf {t}^{\alpha }:=\mathrm{d}u^{\alpha }/\mathrm{d}t\) is tangent to the curves and \(\mathbf {t}^{\alpha }\partial _{\alpha }t=1.\) For any system of coordinates \(u^{\alpha }=u^{\alpha }(x^{\grave{\imath }},t),\) there are defined the vector \(\mathbf {t }^{\alpha }:=(\partial u^{\alpha }/\partial t)_{x^{\grave{\imath }}}\) and the (tangent) vectors \(e_{~\grave{\imath }}^{\alpha }:=(\partial u^{\alpha }/\partial x^{\grave{\imath }})\); and the Lie derivative along \(\mathbf {t} ^{\alpha }\) results in \(\pounds _{t}e_{~^{\grave{\imath }}}^{\alpha }=0.\)

**lapse function**\(\breve{N} (u)>0\) is defined as a positive scalar field which ensues from the fact that the unit d-vector \(\mathbf {n}\) is a unit one; see (16). We use an “inverse hat” in order to distinguish such a symbol

*N*is used traditionally in the literature on GR [39] but, in another turn, the symbol \(N_{i}^{a}\) is used traditionally for the N-connection. We write

**shift**functions (a 3-vector \(\breve{N}^{\grave{\imath }}(u),\) or a d-vector \({\breve{\mathbf {N}}}^{\grave{\imath }}(u)\)). It is useful to define the unit normal \(\breve{n}^{\alpha }\) to the hypersurfaces when \(\breve{n} _{\alpha }=-\breve{N}\partial _{\alpha }t\) and \(\breve{n}_{\alpha }e_{~^{ \breve{\imath }}}^{\alpha }=0.\) In N-adapted form, we can consider that \( \breve{n}_{\alpha }\) is a normalized version of \(\mathbf {n}\) used in (20). This allows us to consider the decompositions

#### 2.2.2 Induced 3-d hypersurface ‘preferred’ linear connections

**extrinsic curvature d-tensors)**of hypersurface \(\Xi \)

### 2.3 Important formulas on space-like N-adapted hypersurfaces

Let us consider 3-surfaces \(\Xi _{t}\) enabled with Riemannian d-metrics when the normal d-vector \(\mathbf {n}\) is time-like. We follow a 4-d point of view treating d-tensor fields defined on any \(\Xi \) as they are defined for \((\mathbf {V},\mathbf {g,N}).\) This avoids the obligation to introduce special frame/coordinate systems and complicated notations depending on double fibration parameterizations etc.

**matter energy density**is defined

**matter momentum density**is

**stress d-tensor**is the bilinear form

#### 2.3.1 Einstein equations in nonholonomic variables for double \(2+2\) and \(3+1\) splitting

#### 2.3.2 Weyl’s tensor \(3+1\) projections adapted to nonholonomic \(2+2\) splitting

Taking any time-like unit vector \(\mathbf {v}^{\alpha }\), we can define a projection tensor, \(\mathbf {h}_{\alpha \beta }=\mathbf {g}_{\alpha \beta }+ \mathbf {v}_{\alpha }\mathbf {v}_{\beta }.\) A general d-vector \(\mathbf {v} _{\alpha }\) is necessary for studying relativistic thermodynamic and hydrodynamic models; see Refs. [7, 9, 25, 31, 33, 34, 35, 37, 39]. For constructions in this work, we can consider \(\mathbf {v}_{\alpha }=\mathbf {n} _{\alpha }\) and use a 3-d hypersurface metric \(\mathbf {q}_{\alpha \beta }= \mathbf {g}_{\alpha \beta }+\mathbf {n}_{\alpha }\mathbf {n}_{\beta }.\)

Equations (25) and (26) are important for constructing the thermodynamical values for gravitational fields following the CET model [40].

## 3 Geometric evolution of Einstein gravitational fields

Nonholonomic Ricci flows for theories with distinguished connections were considered in [20, 21]. To study general relativistic geometric flows and elaborate on thermodynamical models we use a N-adapted \(3+1\) decomposition for the canonical d-connection, \(\widehat{ \mathbf {D}}=(\, _{\shortmid }\widehat{\mathbf {D}},\ ^{t}\widehat{D})\) and d-metric \(\mathbf {g}:=(\mathbf {q,}\breve{N})\) of a 4-d spacetime \(\mathbf {V }\). In this section we formulate the general relativistic geometric flow theory in nonholonomic variables with double splitting. The fundamental functionals and Ricci flow evolution equations are constructed on 4-d Lorentz manifolds determined by exact solutions in GR.

### 3.1 Distortion relations on induced linear connections

### 3.2 Nonholonomc Perelman’s functionals on 3-d hypersurfaces

In order to find explicit solutions of (28) for \(q_{\grave{\imath } \grave{j}}\subset g_{\alpha \beta }\) with \(g_{\alpha \beta }\) defined also as a solution of a 4-d Einstein equations (12), we have to consider a nontrivial \(\grave{r}.\) We can re-write (1) in any nonholonomic basis using the geometric evolution of frame fields, \(\ \partial _{\chi }e_{\grave{\imath }}^{\ \underline{\grave{\imath }}}=q^{ \underline{\grave{\imath }}\underline{\grave{j}}}\, _{\shortmid }R_{\underline{ \grave{j}}\underline{\grave{k}}}e_{\grave{\imath }}^{\ \underline{\grave{k}} }, \) when \(q_{\grave{\imath }\grave{j}}(\tau )=q_{\underline{\grave{\imath }} \underline{\grave{j}}}(\tau )e_{\grave{\imath }}^{\ \underline{\grave{\imath }} }(\tau )e_{\grave{j}}^{\ \underline{\grave{j}}}(\tau )\) for \(e_{\grave{\imath }}(\tau )=e_{\grave{\imath }}^{\ \underline{\grave{\imath }}}(\tau )\partial _{ \underline{\grave{\imath }}}\) and \(e^{j}(\tau )=e_{\ \underline{\grave{j}} }^{j}(\tau )\mathrm{d}x^{\underline{\grave{j}}}.\) There is a unique solution for such systems of linear ODEs for any \(\tau \in [0,\tau _{0}).\)

*f*satisfies \(\int _{\widehat{\Xi }_{t}}M\sqrt{ |q_{\grave{\imath }\grave{j}}|}\mathrm{d}\grave{x}^{3}=1\) for \(M=( 4\pi \tau ) ^{-3}e^{-f}\) . The functionals \(\, _{\shortmid }\widehat{\mathcal {F} }\) and \(\, _{\shortmid }\widehat{\mathcal {W}}\) transform into standard Perelman functionals on \(\widehat{\Xi }_{t}\) if \(\, _{\shortmid }\widehat{ \mathbf {D}}\rightarrow \, _{\shortmid }\nabla .\) The W-entropy \(\, _{\shortmid }\widehat{\mathcal {W}}\) is a Lyapunov type non-decreasing functional.

### 3.3 Nonholonomic Ricci flow evolution equations for 3-d hypersurface metrics

Considering the dependencies of Eqs. (29) and (30) on a smooth parameter \(\chi (\tau )\) for which \(\partial \chi /\partial \tau =-1\) (when, for simplicity, the normalization terms are not included) one can prove the geometric evolution equations for any induced 3-d metric \(\mathbf { q}\) and canonical d-connection \(\, _{\shortmid }\widehat{\mathbf {D}}.\) A subclass of geometric flow models with general relativistic extension from 3-d to 4-d can be elaborated if one of the parameters \(\chi \) or \(\tau \) is taken to be proportional to the time-like fourth coordinate, *t*.

The system of equations (31) and (32) is equivalent to (28) up to a certain redefinition of nonholonomic frames and variables. We have to consider (32) as additional constraints because in nonholonomic variables the Ricci d-tensor is (in general) nonsymmetric. If we do not impose such constraints, the geometric evolution goes with nonsymmetric metrics.

### 3.4 Geometric evolution to 4-d Lorentz configurations as exact solutions in GR

*t*, we introduce such 4-d functionals,

We emphasize that the functionals \(\widehat{\mathcal {F}}\) and \(\widehat{ \mathcal {W}}\) for 4-d pseudo-Riemannian metrics are not of entropy type like in the 3-d Riemannian case. Nevertheless, they describe nonlinear general relativistic diffusion-type processes if \(\mathbf {q}\subset \mathbf {g}\ \) and \(_{\shortmid }\widehat{\mathbf {D}}\) \(\subset \widehat{\mathbf {D}}\) are determined by certain lapse and shift functions as certain solutions of the 4-d gravitational equations. This is motivation to construct such functionals using nonholonomic variables.

*h*- and

*v*-splitting for \(\mathbf {\widehat{\mathbf {D}},}\)

## 4 Generation of off-diagonal solutions

^{7}

### 4.1 Decoupling of Einstein equations for nonholonomic \(2+2\) splitting

**decoupling property,**

^{8}

*t*, we have to consider generating functions for which \(\Psi ^{*}\ne 0.\) We obtain a system of nonlinear PDEs with effective cosmological constant \(\Lambda ,\)

### 4.2 The Levi-Civita conditions

### 4.3 General solutions for (non) holonomic Einstein manifolds

Summarizing the results obtained in previous subsections, we can construct the quadratic linear elements for generic off-diagonal metrics defining 4-d Einstein spaces with an effective cosmological constant \(\Lambda \) and nonholonomic deformations to general sources of type (42).

#### 4.3.1 Solutions with nonholonomically induced torsion

*torsRs*, are written

*h*-metric \( e^{\psi }\) is any solution of the 2-d Poisson equation (46) with source \(\widetilde{\Upsilon }.\) The vertical conformal factor \(\omega (x^{i},y^{3},t)\) can be determined as a solution of (50). The subclass of solutions (57) with Killing symmetry on \(\partial _{3}\) can be extracted for \(\omega ^{2}=1.\)

It should be noted that the effective source \(\Upsilon \) determines an effective source (52) up to a class of frame transforms \(e_{\ \alpha }^{\alpha ^{\prime }}(x^{i},y^{a}).\) Such coefficients must be defined from a system of quadratic algebraic equations for any prescribed \(\Upsilon _{\beta }^{\alpha }=[ \ \tilde{\Upsilon }\delta _{j}^{i},\ \Upsilon \delta _{b}^{a}] .\) The coefficients \(e_{\ \alpha }^{\alpha ^{\prime }} \) and the integration functions \(\, _{1}n_{k}(x^{i})\) and \(_{2}\widetilde{n }_{k}(x^{i})\) can be defined in explicit form if we choose the respective boundary/asymptotic conditions, or solve (for another type of solutions) the Cauchy problem.

The solutions (57) can be parameterized in certain forms generating nonholonomically deformed black ellipsoid, black hole, wormhole, solitonic, and inhomogeneous solutions in various MGTs and in GR; see the discussion and examples in [41, 42, 47, 48].

#### 4.3.2 LC-varieties for effective Einstein manifolds

There are such generating functions and sources when, for instance, black ellipsoid/hole de Sitter configurations can be extracted from (58) in the limit of certain small off-diagonal deformations; for details see [41]. We note that the metrics are generic off-diagonal if the anholonomic coefficients \(\ W_{\alpha \beta }^{\gamma }\) (5) are not zero.

### 4.4 Off-diagonal deformations of physically important solutions in GR

In this section, we present four classes of exact solutions generated by the AFDM. The are constructed explicit examples of generic off-diagonal metrics (58) with parameterizations of the generating and integration functions and constants, and corresponding sources, when certain “prime” metrics in GR are transformed into “target” metrics with modified physical constants (running type, or effective polarizations) and/or deformed horizons and/or self-consistent interactions, for instance, with gravitational solitonic waves.

#### 4.4.1 Ellipsoid Kerr–de Sitter configurations

*p*,

*q*are related to the total black hole mass, \(m_{0}\) and the total angular momentum, \(am_{0},\) for the asymptotically flat, stationary, and axisymmetric Kerr spacetime. The formulas \(m_{0}=Mp^{-1}\) and \(a=Mqp^{-1}\) when \( p^{2}+q^{2}=1\) imply \(m_{0}^{2}-a^{2}=M^{2}.\) In such variables, the vacuum Kerr solution can be written

#### 4.4.2 Nonholonomically deformed wormhole configurations

*B*(

*r*) and

*b*(

*r*) are called, respectively, the red-shift and form functions. On holonomic wormhole solutions, we refer the reader to [52, 53, 54, 55]. There the local coordinates \(u^{\alpha }=(r,\theta ,t,\varphi )\) are used. The radial coordinate has the range \(r_{0}\le r<a.\) The minimum value \(r_{0}\) is for the wormhole throat. The constant

*a*is the distance at which the interior spacetime joins to an exterior vacuum solution (\(a\rightarrow \infty \) for specific asymptotically flat wormhole geometries). The coefficients of the diagonal stress-energy tensor

*M*is a constant mass parameter. For diagonal configurations, we can identify \( \Lambda \) with the effective cosmological constant.

*h*-coordinates when \((r,\theta )\rightarrow (\xi ,\vartheta )\) with \(\xi \) and \(\vartheta \) of length dimension. The data for this primary metric are written

#### 4.4.3 Solitonic waves for inhomogeneous cosmological solutions

*s*-label) generating function \( \tilde{\Psi }=\ ^{s}\tilde{\Psi }(r,t)=4\arctan e^{q\sigma (r-vt)+q_{0}}\) and construct a metric

In the absence of matter, the off-diagonal cosmology is completely determined by \(\ \Upsilon \) related to an effective cosmological constant induced by geometric flows. Such configurations can be determined alternatively using distribution of matter fields when contributions from massive gravity are with small anisotropic polarization; for details see [57, 58, 59, 60].

#### 4.4.4 Off-diagonal deformations of FLRW metrics and gravitational solitonic waves

*v*-subspace together with self-consistent off-diagonal propagation of such waves via \(w_{i}=\widetilde{A}^{\bullet }.\) More general 3-d solitonic gravitational waves are possible which can propagate self-consistently in Minkowski spacetime or in a FLRW background. To generate such solutions we need to take a generating function \(\ ^{s}\Psi (x^{1},x^{2},t)\) which is a solution of the Kadomtsev–Petviashvili (KdP) equation [61, 62, 63].

If we consider that in the ansatz of type (58) \(y^{3}=t\) (time-like coordinate) and \(y^{4}=\varphi \) (an angular space coordinate), we construct stationary solutions with Killing symmetry on \(\partial _{3};\) see the details in [41, 42]. Such solutions in GR and geometric flow theory include as particular cases black ellipsoid configurations, Taub NUT configurations, and other types of Coulomb-like gravitational fields. In particular, for small \(\varepsilon \)-deformations they include black hole and black ellipsoid solutions in GR and certain classes of modified theories. Such gravitational configurations are characterized by different thermodynamic values in a W-thermodynamic model of geometric flows and their stationary Ricci soliton configurations.

## 5 Nonholonomic thermodynamics of gravitational fields

There is a standard theory of the thermodynamics of the black hole (BH) solutions originally elaborated by Bekenstein–Hawking constructions for stationary solutions in gravity theories (for a review, see [39] and the references therein). Following the formalism of double fibrations, the BH thermodynamics can be derived for a very special example of Lyapunov-type functionals on 3-d hypersurfaces with further \(2+1\) splitting (or \(2+1+1\) holonomic fibrations with horizon configurations and corresponding asymptotic conditions). In general, we cannot apply the BH thermodynamics to study general gravitational configurations, for instance, models of inhomogeneous cosmology and/or other spacetime configurations in GR and MGTs. Certain ideas were proposed to formulate more general thermodynamic descriptions of gravitational fields; see [40] (for the so-called CET model) and the references therein.

In this section, we develop a W-functional thermodynamic model on a 3-d closed space-like hypersurface in GR, following the standard theory of Ricci flows. In general, such an approach is very different from that considered in standard BH thermodynamics. As a matter of principle, it is possible to establish certain equivalence conditions (with very special holonomic vacuum gravity configurations or diagonal de Sitter BH solutions) when the W-functional approach will give the same result as in Bekenstein–Hawking BH thermodynamics. The goal of this section is to elaborate on models on nonholonomic thermodynamics of gravitational fields using 4-d generalizations of Perelman’s W-functionals. We shall also speculate how such constructions can be related to the CET approach if certain additional conditions are imposed. In this work, we restrict our approach to general relativistic flows of the 3-d to the 4-d configuration to a special class of models when the effective temperature \(\beta ^{-1}(t)\) depends, in general, on the time-like coordinate *t*.

### 5.1 General relativistic models of W-entropy and geometric flow evolution

We emphasize that Perelman’s functional \(\, _{\shortmid }\mathcal {W}\) (30) is in a sense analogous to minus the entropy. Similar values can be considered for various metric compatible nonholonomic Ricci flows and (non) commutative, fractional derivative and other type modifications [8, 9, 20, 21]. This allows us to associate certain analogous thermodynamical values characterizing a (non) holonomic modified Ricci flow evolution of the metrics with a local Euclidean structure and generalized connections. Using \(\, _{\shortmid }\mathcal {W}\) for \(( \mathbf {q},\, _{\shortmid }\widehat{\mathbf {D}})\) and its 4-d generalization \(\widehat{\mathcal {W}}\) in the form (34), or (36) for \((\ \mathbf {g},\widehat{\mathbf {D}}),\) we can construct relativistic geometric evolution models with generalized Hamilton equations of type (38).

*t*of any family of closed hypersurfaces all determined by \(\, _{\shortmid }\widehat{\mathbf {D}}\),

### 5.2 W-thermodynamic values for exact solutions in GR

For nonholonomic 4-d Lorentz–Ricci solitonic equations defined by systems of type (57), or (58), the generating function \(\Psi (x^{k},t)\) (or \(\widetilde{\Psi }(x^{k},t),\) or \(\check{\Psi }(x^{k},t)\) for torsionless configurations) and the effective source \(\Upsilon (x^{k},t)\) can be prescribed in some forms not depending one on another. The vertical conformal factor \(\omega \) can be an arbitrary function on \((x^{k},y^{3},t)\) subjected to the conditions (50). Such values should be subjected to an additional constraint if we consider that the 4-d solutions for a d-metric \(\mathbf {g}\) encode also 3-d d-metrics \(\mathbf {q}\). The 3-d metric is parameterized in the form (40) with a Ricci flow evolution determined by the Hamilton equations (28) on a relativistic parameter. To construct explicit solutions, we consider the parameter \(\chi =t\) for 3-d evolution equations written with respect to N-adapted frames.

#### 5.2.1 Modified 3-d Ricci flows with induced nonholonomic torsion

#### 5.2.2 Modified 3-d Ricci flows of LC-configurations

#### 5.2.3 N-adapted 3-d Ricci flows on exact solutions in GR

#### 5.2.4 Relativistic thermodynamic values for N-adapted 3-d modified Ricci flows

*t*of any family of closed hypersurfaces. We can decide if certain solutions with an effective Lorentz–Ricci soliton source and/or with contributions from additional MGT sources may be more convenient thermodynamically than other configurations.

It is possible to define and compute thermodynamic like values (69) for generic off-diagonal solutions in GR as we explained for solutions (58) and corresponding functionals \(\tilde{\Psi }[\check{ \Psi }],\Theta [\check{\Psi }]\) and \(\omega [\check{\Psi }].\) We emphasize that in both cases with zero, or non-zero nonholonomic torsion, the above formulas for thermodynamical values are defined for a non-zero effective \(\widetilde{\Lambda }\) and non-zero source \(\Upsilon .\) For (effective) vacuum configurations, such formulas have to be computed using corresponding classes of off-diagonal solutions.

The entities (68) and/or (69) can be computed for 4-d configurations determined by modified Lorentz–Riemann solitons, \(\widehat{ \mathcal {E}}=\int _{t_{1}}^{t_{2}}\mathrm{d}t\, _{\shortmid }\widehat{\mathcal {E}},\) \( \widehat{\mathcal {S}}=\int _{t_{1}}^{t_{2}}\mathrm{d}t\, _{\shortmid }\widehat{S},\) \( \widehat{{\Sigma }}=\int _{t_{1}}^{t_{2}}\mathrm{d}t\, _{\shortmid }\widehat{\sigma }\) determined by \(_{\shortmid }\widehat{\mathbf {D}}.\) In a similar form, we can use the distortion formulas (27) and compute \(\ ^{\nabla }\mathcal {E} =\int _{t_{1}}^{t_{2}}\mathrm{d}t\, _{\shortmid }^{\nabla }\mathcal {E},\ ^{\nabla } \mathcal {S}=\int _{t_{1}}^{t_{2}}\mathrm{d}t\, _{\shortmid }^{\nabla }S,\ ^{\nabla }{ \Sigma }=\int _{t_{1}}^{t_{2}}\mathrm{d}t\, _{\shortmid }^{\nabla }\sigma \) for \(\, _{\shortmid }\nabla .\) Such values are positively different for \(\, _{\shortmid }\widehat{\mathbf {D}}\rightarrow \, _{\shortmid }\nabla \) for certain topologically nontrivial configurations. As a result, we can analyze if a nonholonomic configuration with N-adapted \(_{\shortmid }\widehat{ \mathbf {D}}\) may be more, or less, convenient thermodynamically than a similar holonomic one as determined by \(\, _{\shortmid }\nabla .\)

Finally, we note that geometric thermodynamics values (68) are defined both for (modified) black hole solutions and inhomogeneous cosmological solutions. The physical meaning of such a thermodynamical approach is very different from that of standard black hole thermodynamics in GR. Nevertheless, certain criteria for equivalent modeling can be analyzed in various MGTs; see [42, 56, 57, 58, 59, 60, 62].

### 5.3 General relativistic hydrodynamics and thermodynamics for geometric flows of gravitational fields

The thermodynamic quantities (64) and (65) are formulated in terms of variables with coefficients computed with respect to N-adapted frame of reference which allows extensions of 3-d thermodynamic values to 4-d ones. This is a hidden aspect of models of non-relativistic hydrodynamics and an apparent property of relativistic theories; see modern approaches in [32, 33, 34, 35, 36, 37]. In this section, we speculate on a model of geometric flows with local thermodynamic equilibrium for which there exists a single distinguished velocity field \(\mathbf {v}_{\alpha }\) (if it is convenient, we can take \(\mathbf {v} _{\alpha }=\mathbf {n}_{\alpha }),\) and a corresponding N-adapted rest frame, where all flow evolutions of the related physical quantities are described by simple formulas.

*W*-entropy) together with a non-zero particle production. In such a case, we must introduce a term like \(\widehat{\mathcal {S}} _{0}^{\alpha }=\widehat{S}_{0}\mathbf {v}^{\alpha }+\widehat{\mathcal {J}} _{0}^{\alpha }\) with an entropy current \(\widehat{\mathcal {J}}_{0}^{\alpha }\) determined by geometric flows and \(\widehat{S}_{0}\) identified with the standard black hole entropy. Therefore the diffusion current density \( \widehat{j}^{\alpha }\) consists of the dissipative part of the particle number (and the momentum density/energy) currents. This defines the difference of the total and the equilibrium pressure \(\Pi ^{\alpha \beta }=\widehat{ \mathcal {P}}^{\alpha \beta }+p_{0}\mathcal {\pi }^{\alpha \beta }.\) The effective viscous pressure determines the dissipative parts of the energy momentum.

It should be mentioned that a splitting into some dissipative and non-dissipative parts of certain physical quantities is related to and depends on the local rest frame (how it is chosen and N-adapted). Additionally to the velocity field of the geometric flow continuum, this requires a particular thermostatics to determine the static pressure. However, the dissipation of thermodynamical systems (in our approach, by general relativistic Ricci flows) is principally defined by the entropy production. This is implicitly related to the background thermostatics, which is a concept for systems in local equilibrium. On the other hand, the rest frame is not determined in the case of dissipation, neither by any special form of the physical quantities. For geometric flows related to 4-d exact solutions in GR, one may consider to extend the Perelman thermodynamic approach by additional construction with the velocity field. We have to address nonholonomic kinetic theory and possible Finsler-like modifications of GR, relativistic thermodynamics, and diffusion as in Refs. [7, 8, 9]. Such models are planned to be elaborated in our further work.

Finally, the main conclusion is that we can characterize the gravitational field equations by Perelman’s W-entropy on any closed 3-d hypersurface. In such a case, a natural statistical thermodynamic model can be associated. To extend the approach in a 4-d general relativistic form it is necessary to elaborate on modified relativistic thermodynamic and hydrodynamic theories, which is the main purpose of this work. The constructions can be performed in explicit form and related to general classes of exact solutions in GR if we formulate all gravitational field, geometric evolution, and effective relativistic thermodynamic theories in certain N-adapted nonholonomic variables. In the next section, we show how this can be connected to exact solutions.

### 5.4 Parameterizations for the CET model

^{9}For perfect (pressureless) matter, \(\mathbf {T}_{\alpha \beta }=p\mathbf {g}_{\alpha \beta }+(\rho +p) \mathbf {v}_{\alpha }\mathbf {v}_{\beta },\) where \(\mathbf {v}_{\alpha }\mathbf { v}^{\alpha }=-1\) , \(\rho \), and

*p*are, respectively, the density and pressure. The 4-velocity of the fluid can be taken as \(v^{\alpha }=(0,0,0,1) \) in a certain co-moving N-adapted frames when \(\mathbf {T} _{~\beta }^{\alpha }=\mathrm{diag}[0,0,0,-\rho ].\) We can consider also fluids with nontrivial momentum density \(\mathbf {q}^{\alpha }\) and anisotropic (tracefree) pressure \(\pi _{\alpha \beta },\) when

^{10}

*V*is the spatial volume. For the vacuum gravitational fields, we consider the quantities

*f*on a 3-dimensional closed hypersurface can be considered as a function determining the natural log of partition function \( Z=\int e^{-\beta E}\mathrm{d}\omega (E),\) with density of states measure \(\omega (E),\)

In explicit form, the effective entropy of the gravitational fields and thermodynamic transforms should be defined differently, for instance, for the Coulomb and/or wave-like gravitational fields, when the respective constants \(\hat{\alpha }\) and \(\hat{\beta }\) are chosen so as to obtain equivalent models for \(~^{g}S\) and/or *S*. Prescribing any values for independent data \( ~^{g}S\) and \(~^{g}\mathcal {T}\), we can construct *S* and \(\log Z\) using, respectively, Eqs. (77) and (78). We denote the solution of the last equation in the form \(\log ~^{g}Z.\) Inverting Eq. (76), we can find a corresponding function \(f=~^{g}f\) describing the geometric evolution of a configuration of gravitational fields characterized by certain relativistic thermodynamics data \( (~^{g}S,~^{g}\mathcal {T}).\)

In [1], the W-entropy was defined by analogy to statistical thermodynamics but a microscopic description was not considered. In statistical mechanics, the partition function \(Z=\sum \nolimits _{i}e^{-\beta E_{i}}\) for a thermodynamic system is \(\Gamma [\varphi _{i},E_{i},\beta ]\) in a canonical ensemble with the \(E_{i}\) being the energies associated with corresponding “microstates” \(\varphi _{i}\) at inverse temperature \(\beta \) (we consider summation on all available “microstates”). For non-discrete microstates, one considers integrals over the spaces of microstates \(\Omega ,\) \(Z=\int \nolimits _{\upsilon }e^{-\beta E(\omega )}\mathrm{d}\omega ,\) with associated energy functions \(E:\Omega \rightarrow \mathbb {R }\) and \(\mathrm{d}\omega \) being the density of states measure on \(\Omega .\) The entropy *S* (77) of \(\Gamma \) was computed for equilibrium states at temperature \(\tau .\) In the relativistic case, we can consider such constructions for an effective theory for the evolution of certain 3-d metrics embedded into 4-d spacetime for which a local gravitational equilibrium exists for a time-like variable *t*. As a thermodynamic system, the analogous \(\Gamma \) is characterized by a full set of “macrostates” describing its large-scale properties and equivalently modeled by the data \(~^{g}S\) and \(~^{g} \mathcal {T}\).

It should be noted that Perelman called *f* the dilaton field and used also an *F*-functional, \(F=-\tau \log Z,\) with a “first variation” formula which “can be found in the literature on string theory, where it describes the low energy effective action; \(\ldots \)” see the end of Sect. 1 in [1]. Recently, the analogy with string theory in the Polyakov formulation [69] was exploited in Ref. [22], where a general scheme of defining partition functions associated to relevant geometric flows was proposed. The Lin approach is based on the functional determinant of differential operators and has well-defined microstates as members of a functional space. For each microstate, it associates the “Dirichlet energy” which in turn is associated to the underlying operator. Using double, \(3+1\), and \(2+2\) fibrations, the corresponding assumptions and data (on analogous macroscopic thermodynamical values associated to solutions of the Einstein equations, additional smooth functions etc.) we can determine the operator for energy determination or macrostates.

## 6 Final remarks and conclusions

Perelman’s proof of the Poincaré conjecture provided a fundamental result on the topological structure of the Universe. He elaborated a general schematic procedure in geometric analysis and speculated on a number of perspectives for applications in modern physics. A statistical and thermodynamic analogy was developed for geometric evolution scenarios using Lyapunov-type functionals. The approach was based on the concept of W-entropy. It was supposed from the very beginning [1] that geometric flows may have certain implications for black hole physics and string theory but the original theory of Ricci evolution flows was formulated in a non-relativistic form. So, Perelman’s ideas could not be developed in a framework of theories with geometric flow evolution of 3-d Riemannian metrics.

This article has a very exact goal: to understand the W-entropy in a wide range of general relativistic geometric flows and analyze possible connections to other formulations of gravitational thermodynamics describing general nonhomogeneous cosmological solutions and black hole configurations. To this end, we need to provide a satisfactory relativistic account of analogous statistical thermodynamical models associated to geometric flows of exact solutions in GR resulting in effective polarizaton (running) of the fundamental constant and generic off-diagonal effects. This will remain a challenge with many interesting directions in MGTs and modern accelerating cosmology emerging from the work presented here. An interesting problem is that, for instance, certain scenarios in modern cosmology can be modeled equivalently by generic off-diagonal interactions in GR and/or by analogous solutions in a MGT. Nevertheless, such gravitational field configurations have very different properties in a framework of geometric flow theory, considering its self-similar configurations as (relativistic) Ricci solitons. The corresponding analogous thermodynamics is determined, in general, by different types of physical values. This motivates our approach to study general relativistic models of Ricci flow evolution of exact solutions in gravity theories.

In this paper, we have shown in explicit form how the W-entropy can be generalized for relativistic geometric evolution of solutions of the Einstein equations. This allows for a statistical thermodynamic description of gravitational interactions, their (fractional) diffusion and kinetic processes [7, 8, 9]. The marriage of the analogous Perelman’s thermodynamics and GR is an issue of very active debates on physical meaning of such constructions and new mathematics. A temperature-like evolution parameter can be considered also for relativistic generalizations but we cannot address the problem as a specific type heat propagation in the context of relativistic dynamics of a non-perfect fluid like in various approaches to relativistic thermodynamics, nonlinear diffusion and relativistic kinetic theory [32, 33, 34, 35, 36, 37]. In theories with geometric flows, we consider the evolution of metrics and fundamental geometric objects (in general, these can be certain generalized connections, curvatures, and torsions). Similar to heat fluxes, we can consider non-relativistic gradient flows and consider an unbounded speed of effective thermal disturbances (fluctuations of tensor fields). This is due to the parabolic nature of PDEs describing the heat transport. In the relativistic cases, we get not only an inconvenience but indeed a fundamental problem. Various issues were studied related to this problem in relativistic hydrodynamical and dissipative theories [25, 26, 27, 28, 29, 31] (for a review, see [38]).

Such constructions, in a macroscopic relativistic thermodynamic formulation [40], seem to be important for the structure formation of Universes, black hole thermodynamics, and the characterization of nonlinear waves, locally anisotropic and/inhomogeneous gravitational configurations. It is possible to formulate an underlying operator formalism and microscopic approach in the spirit of Polyakov’s approach to string theory. This scheme requires a method of constructing generic off-diagonal solutions depending on all spacetime variables [41, 42] which drive in nonlinear parametric form the relativistic Ricci flows evolution of the 3-d hypersurface metrics in a 4-d spacetime.

We conclude that the anholonomic frame deformation method involved in our constructions can be applied to a wide range in GR and MGTs [59, 60, 70, 71, 72, 73, 74] and generalized geometric evolution models [19, 20, 21]. Such constructions are more general and different from those elaborated in [75, 76] where Ricci flows were studied in connection with the standard black hole thermodynamics and possible extensions to quantum diffusion and informational entropy.

## Footnotes

- 1.
Remark 5.3 is interesting in [1] (and the next paragraph, just before Sect. 6 in that paper) which we reproduce here: “An entropy formula for the Ricci flow in dimension two was found by Chow ...; there seems to be no relation between his formula and ours. ... The interplay of statistical physics and (pseudo)-riemannian geometry occurs in the subject of Black Hole Thermodynamics, developed by Hawking et al. Unfortunately, this subject is beyond my understanding at the moment.”

- 2.
The left labels 3 and 1 for

*V*will be used always when it is important to state that a \(3+1\) splitting is considered with three space-like and one time-like local coordinates. - 3.
In this work, we use the following conventions: local coordinates for a \(2+2\) splitting are denoted \(u^{\mu }=(x^{i},y^{a}),\) (in brief, we shall write \( u=(x,y)\)), where indices run, respectively, over values of type \(i,j,\ldots =1,2\) and \( a,b,\ldots =3,4.\) The small Greek indices run over values \(\alpha ,\beta ,\ldots =1,2,3,4\) considering that \(u^{4}=y^{4}=t\) is a time-like coordinate. An arbitrary local basis will be denoted by \(e^{\alpha }=(e^{i},e^{a})\) and the corresponding dual one, the co-basis, is \(e_{\beta }=(e_{j},e_{b}).\) There are always nontrivial frame transforms to corresponding coordinate bases, \( \partial _{\alpha ^{\prime }}=(\partial _{i^{\prime }},\partial _{a^{\prime }})\) [for instance, \(\partial _{i^{\prime }}=\partial /\partial x^{i^{\prime }}],\) and co-basis \(\mathrm{d}u^{\alpha ^{\prime }}=(\mathrm{d}x^{i^{\prime }},dy^{a^{\prime }}),\) when \(e_{\beta }=A_{\beta }^{\ \beta ^{\prime }}\partial _{\beta ^{\prime }}\) and \(e^{\alpha }=A_{\ \alpha ^{\prime }}^{\alpha }(u)\mathrm{d}u^{\alpha ^{\prime }}\) are arbitrary frame (vierbein) transforms. We shall use also various types of primed, underlined indices etc. The Einstein summation rule on repeating upper–lower indices will be applied if the contrary will be not stated.

- 4.
We can elaborate a N-adapted covariant and/or local differential and integral calculus and a corresponding variational formalism in GR using the N-elongated operators (3) and (4). The geometric constructions are performed for distinguished objects, in brief, d-objects with coefficients determined with respect to N-adapted (co) frames and their tensor products. A vector \(Y(u)\in T\mathbf {V}\) can be parameterized as a d-vector, \(\mathbf {Y}=\) \(\mathbf {Y}^{\alpha }\mathbf {e}_{\alpha }= \mathbf {Y}^{i}\mathbf {e}_{i}+\mathbf {Y}^{a}e_{a},\) or \(\mathbf {Y}=(hY,vY),\) with \(hY=\{\mathbf {Y}^{i}\}\) and \(vY=\{\mathbf {Y}^{a}\}.\) Similarly, we can determine and compute the coefficients of d-tensors, N-adapted differential forms, d-connections, d-spinors etc. All fundamental geometric and physical equations can be re-written equivalently in N-adapted frames; for details see [41].

- 5.
We use abstract left labels

*A*and*m*in order to distinguish the values from similar notations, for instance, \(\widehat{\mathbf {T}}_{\ \alpha \beta }^{\gamma }.\) - 6.
- 7.
- 8.
- 9.
Such formulas are similar to those for \(\nabla \) if we consider the distorting relations \(\widehat{\mathbf {D}}=\nabla +\widehat{\mathbf {Z}}\) to be uniquely determined by the data \((\mathbf {g,N})\) and when \(\widehat{\mathbf {D}}_{\mid \widehat{\mathbb {T}}=0}\rightarrow \nabla .\)

- 10.
For the temperature, we use the symbol \(\mathcal {T}\) instead of

*T*, or*t*, in order to avoid possible ambiguities with similar notations, respectively, for the tangent space,*TV*, the time-like coordinate,*t*, etc.

## Notes

### Acknowledgements

SV was supported by a travel grant from MG14 at Rome and reports certain research related to his basic activity at UAIC, a DAAD fellowship and the Program IDEI, PN-II-ID-PCE-2011-3-0256. Possible implications in modern cosmology and geometric mechanics of such geometric methods were discussed with N. Mavromatos, E. Saridakis, and P. Stavrinos. He is grateful for DAAD hosting to D. Lüst and O. Lechtenfeld.

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