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Thermodynamics and Decay of de Sitter Vacuum

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A peer-reviewed article of this preprint also exists.

Grigory E. Volovik^*

This version is not peer-reviewed

Submitted:

28 May 2024

Posted:

28 May 2024

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Abstract

We discuss the consequences of the unique symmetry of the de Sitter spacetime. This symmetry leads to the specific thermodynamic properties of the de Sitter vacuum, which produces the thermal bath for matter. The de Sitter spacetime is invariant under the modified translations, ${\bf r}\rightarrow {\bf r} -e^{Ht}{\bf a}$, where $H$ is the Hubble parameter. For $H\rightarrow 0$, this symmetry corresponds to the conventional invariance of Minkowski spacetime under translations ${\bf r}\rightarrow {\bf r} -{\bf a}$. Due to this symmetry, all the comoving observers at any point of the de Sitter space perceive the de Sitter environment as the thermal bath with temperature $T=H/\pi$, which is twice larger than the Gibbons-Hawking temperature of the cosmological horizon. This temperature does not violate the de Sitter symmetry, and thus does not require the preferred reference frame, as distinct from thermal state of matter, which violates the de Sitter symmetry. This leads to the heat exchange between gravity and matter, and to instability of de Sitter state towards the creation of matter, its further heating, and finally to the decay of the de Sitter state. The temperature $T=H/\pi$ determines different processes in the de Sitter environment, which are not possible in the Minkowski vacuum, such as the process of ionization of an atom in the de Sitter environment. This temperature also determines the local entropy of the de Sitter vacuum state, and this allows us to calculate the total entropy inside the cosmological horizon. The result reproduces the Gibbons-Hawking area law, which is related to the cosmological horizon, $S_{\rm hor}=4\pi KA$, where $K=1/16\pi G$. This supports the holographic properties of the cosmological event horizon. We extend the consideration of the local thermodynamics of the de Sitter state using the $f({\cal R})$ gravity. In this thermodynamics, the Ricci scalar curvature ${\cal R}$ and the effective gravitational coupling, $K$, are thermodynamically conjugate variables. The holographic connection between the bulk entropy of the Hubble volume, and the surface entropy of the cosmological horizon remains the same, but with the gravitational coupling $K=df/d{\cal R}$. Such connection takes place only in the $3+1$ spacetime, where there is the special symmetry due to which the variables $K$ and ${\cal R}$ have the same dimensionality. We also consider the lessons from the de Sitter symmetry for the thermodynamics of black and white holes.

Keywords:

Subject: Physical Sciences - Theoretical Physics

1. Introduction

We consider the local thermodynamics of the de Sitter stage of the expansion of the Universe. The term “local” means that we consider the de Sitter vacuum as the thermal state, which is characterized by the local temperature. This consideration is based on observation, that matter immersed in the de Sitter vacuum feels this vacuum as the heat bath with the local temperature

T = H / π

, where H is the Hubble parameter. This temperature has no relation to the cosmological horizon, and to the Hawking radiation from the cosmological horizon. However, it is exactly twice the Gibbons-Hawking temperature,

T_{GH} = H / 2 π

. The reason for such relation is thel symmetry of the de Sitter space-time with respect to the combined translations. In the Minkowski vacuum, this symmetry becomes the conventional invariance of under translations.

The existence of the local temperature suggests the existence of the other local thermodynamic variables, which participate in the local thermodynamics of the de Sitter state. In addition to the the local entropy density s and local vacuum energy density

ϵ

, there are also the local thermodynamic variables related to the gravitational degrees of freedom.

Although the local temperature is twice larger than the Gibbons-Hawking temperature assigned to the cosmological horizon, there is the certain connection between the local entropy s and the global entropy usually assigned to the event horizon. It appears that the total entropy of the de Sitter state in the volume

V_{H}

bounded by the cosmological horizon coincides with the Gibbons-Hawking entropy, which is proportional to the area A of the horizon,

s V_{H} = A / 4 G

. Such holographic bulk-surface correspondence takes place only in the

3 + 1

spacetime. Although the peculiarity of the

3 + 1

spacetime may be related to the special symmetry, which connects the local thermodynamic variables, the origin of the holography is still not very clear. That is why we extended the consideration of the local thermodynamics to the

f (R)

gravity, and checked the bulk-surface correspondence in this modified version of general relativity.

The

f (R)

gravity in terms of the Ricci scalar

R

is one of the simplest geometrical models, which describes the dark energy and de Sitter expansion of the Universe.[1,2,3,4,5,6,7] It was used to construct an inflationary model of the early Universe – the Starobinsky inflation, which is controlled by the

R^{2}

contribution to the effective action. This class of models,

f (R) \propto R - R^{2} / M^{2}

, was also reproduced in the so-called q-theory,[8,9] where q is the 4-form field introduced by Hawking[10] for the phenomenological description of the physics of the deep (ultraviolet) vacuum (here the sign convention for

R

is opposite to that in Ref. [2]). The Starobinsky model is in good agreement with the observations. However, despite the observational success, the theory of Starobinsky inflation is still phenomenological. Due to a rather small mass scale M compared with the Planck scale it is difficult to embed the model into a UV complete theory.[11,12,13] But we used this model only for the generalization of the de Sitter thermodynamics and for consideration of the validity of the holographic principle.

The

f (R)

theory demonstrates that the effective gravitational coupling K (it is the inverse Newton constant,

K = 1 / 16 π G

) and the scalar curvature

R

are connected by equation

K = d f / d R

. This suggests that K and

R

are the thermodynamically conjugate variables.[14,15] This pair of the non-extensive gravitational variables is similar to the pair of the electrodynamic variables, electric field

E

and electric induction

D

, which participate in the thermodynamics of dielectrics. They are also similar to the pair of magnetic thermodynamic variables, magnetic induction

B

and magnetic field

H

In the de Sitter spacetime, the local temperature does no depend on the theories of general relativity and thus has the same value

T = H / π

. Using the local thermodynamics with this temperature, we obtained the general result for the total entropy of the Hubble volume,

S_{bulk} = s V_{H} = 4 π K A = A / 4 G = S_{hor}

, where

K = d f / d R

is the effective gravitational coupling and

R = - 12 H^{2}

. This supports the holographic bulk-surface correspondence in the

3 + 1

spacetime.

Note that the

3 + 1

spacetime has special symmetry, which is absent in the other dimensions. The thermodynamically conjugate variables have the same dimensionality of the square of inverse length:

[K] = [R] = [1 / l^{2}]

[B] = [H] = [1 / l^{2}]

and

[D] = [E] = [1 / l^{2}]

. It looks that this symmetry is important for the validity of the holographic correspondence.

Since the de Sitter state has thermal behaviour, it serves as the thermal bath for matter. The matter violates the de Sitter symmetry. As a result the energy exchange between vacuum and matter leads to the decay of the de Sitter state.

The plan of the paper is the following.

In Section 2 we show that the de Sitter vacuum serves as the thermal bath for the external matter – the matter immersed into the de Sitter environment. This is different from the traditional consideration of the vacua of the quantum fields in the de Sitter spacetime, which uses the Euclidean action method. Example of the influence of the de Sitter vacuum to the external matter is provided by an atom in the de Sitter environment (Section 2.1). As distinct from the atom in the flat space, the atom in the de Sitter vacuum has a certain probability of ionization. The rate of ionization is similar to the rate of ionization in the presence of the thermal bath with temperature

T = H / π

.[16,17,18,19,20] In Section 2.2 it is shown that the same temperature determines the other activation processes, which are energetically forbidden in the Minkowski spacetime, but are allowed in the de Sitter background. Examples are the splitting of the heavy particle with mass m to two particles with masses

m_{1} + m_{2} > m

,21,22] and radiation of electron-positron pairs by the electron at rest. In Section 2.4 it is shown that the local temperature T also determines the Gibbons-Hawking temperature of radiation from the cosmological horizon

T_{GH} = T / 2

without using the Euclidean action.

Section 3 is devoted to the local thermodynamics of the de Sitter state, which is determined by the local temperature

T = H / π

. The local temperature leads to the local entropy of the de Sitter thermal bath (Section 3.2), which integrated over the Hubble volume reproduces the Gibbons-Hawking entropy of the cosmological horizon (Sec.Section 3.4).

Section 4 describes the attempt to obtain the de Sitter thermal states from the general principles of thermodynamics of the many-body systems. We consider the multi-metric gravity, which can be viewed as an ensemble of the sub-Universes, each described by its own metric

g_{μ ν (n)}

(or tetrads

e_{μ (n)}^{a}

), by its own gravitational coupling

K_{n}

and cosmological constant

Λ_{n}

. The heat exchange between the sub-Universes leads to their thermalization – the formation of the Universe in which the sub-Universes have the common Hubble parameter and thus they have the common temperature.

Section 5 is devoted to thermodynamics of de Sitter in the

f (R)

gravity. It contains the pair of the thermodynamically conjugate variables, K and

R

(Section 5.1). These variables together with the local temperature and local entropy provide the generalization of Gibbs-Duhem relation for the de Sitter state (Section 5.2). The confirmation of the holographic result for the total entropy of the Hubble volume in the

f (R)

gravity is obtained in Section 5.3:

S_{bulk} = s V_{H} = 4 π K A = S_{hor}

, The quadratic gravity and its symmetry are discussed in Section 5.4.

The Section 6 is devoted to the de Sitter decay due to the thermalization of matter by the de Sitter heat bath, and by the thermal fluctuations of the de Sitter state. These two mechanisms lead to different power laws of the decay, which may correspond two different epochs.

Section 7 and Section 8 demonstrate how the local entropy of the de Sitter state allows us to consider the thermodynamics of the Schwarzschild black hole. The starting point of our consideration in Section 7.3 is that the black hole can be obtained from the relaxation of the gravastar object – the black hole, which has the de Sitter core. It is important that the de Sitter interior of the gravastar is represented by the contracting de Sitter state. The contracting de Sitter in Section 7.2 has negative Hubble parameter

H < 0

, and thus the negative temperature

T = H / π < 0

and negative entropy. The contracting and expanding de Sitter states can be considered as two phases obtained from the symmetric state of the Minkowski vacuum by the spontaneous breaking of the time reversal symmetry. These phases transform to each other under the time reversal,

t \to - t

. In this sense, the Hubble parameter H can be considered as the order parameter of the symmetry breaking phase transition.

Since in the considered gravastar object, the cosmological and black hole horizons cancel each other, the gravastar has zero entropy. In the process of relaxation of the gravastar to the black hole, the de Sitter core with its negative entropy shrinks. This results in the Hawking-Bekenstein entropy of the black hole horizon (Section 7.4). The negative entropy of the white hole is considered in Section 7.5. The heat exchange between black holes in the multi-metric gravity is discussed in Section 7.8. Section 8 provides the alternative derivation of the thermodynamics of black and white holes using the macroscopic quantum tunneling.

Finally the conclusion is in Section 9.

2. De Sitter State as Heat Bath for Matter

2.1. Atom in de Sitter Environment as Thermometer

We consider the de Sitter thermodynamics using the Painlevé-Gullstrand (PG) form,[23,24] where the metric is

d s^{2} = - d t^{2} + {(d r - v (r) d t)}^{2} .

(1)

Here

v (r)

is the shift velocity, which in condensed matter plays the role of the velocity of the superfluid component of matter (velocity of the "superfluid quantum vacuum" [25] ). In the de Sitter expansion the velocity of the "vacuum" is

v (r) = H r

and the metric is

d s^{2} = - d t^{2} + {(d r - H r d t)}^{2} + r^{2} d Ω^{2} .

(2)

The PG metric is stationary, i.e. does not depend on time, and it does not have the unphysical singularity at the cosmological horizon. That is why it is appropriate for consideration of the local thermodynamics both inside and outside the horizon. It also allows us to consider two different phases of the vacuum with broken time reversal symmetry. These are the expanding de Sitter Universe with

H > 0

and the contracting de Sitter Universe with

H < 0

, which transform to each other under the time reversal,

t \to - t

. In this sense, the Hubble parameter H can be considered as the order parameter of the symmetry breaking phase transition from the symmetric state of the Minkowski vacuum.

Now let us consider an atom at the origin,

r = 0

. The atom is the external object in the de Sitter spacetime, which violates the de Sitter symmetry. It plays the role of the detector (or the role of the static observer) in this spacetime. The electron bounded to an atom may absorb the energy from the gravitational field of the de Sitter background and escape from the electric potential barrier. If the ionization potential is much smaller than the electron mass but is much larger than the Hubble parameter,

H ≪ ϵ_{0} ≪ m

, one can use the nonrelativistic quantum mechanics to estimate the tunneling rate through the barrier.

Let us consider electron on the n-th level in the hydrogen atom. Under de Sitter gravitational field this electron can escape from the atom with the conservation of energy, which in the classical limit is given by the classical equation:

\begin{matrix} \frac{p_{r}^{2}}{2 m} + p_{r} v (r) = - E_{n}, E_{n} = \frac{m e^{4}}{2 ℏ^{2}} \frac{1}{n^{2}} . \end{matrix}

(3)

Here

v (r) = H r

and

p_{r} (r) v (r)

is the Doppler shift, which allows for electron to reach the negative energy when it escapes from the atom. The corresponding radial trajectory

p_{r} (r)

for escape of electron from the atom is:

\begin{matrix} p_{r} (r) = - m v (r) + \sqrt{m^{2} v^{2} (r) - 2 m E_{n}} . \end{matrix}

(4)

The integral of

p_{r} (r)

over the classically forbidden region,

0 < r < r_{n} = \sqrt{2 E_{n} / m H^{2}}

, gives the ionization rate

\begin{matrix} w \sim exp (- 2 Im S) = \\ = exp (- 2 \int_{0}^{r_{n}} d r \sqrt{2 m E_{n} - m^{2} H^{2} r^{2}}) = exp (- \frac{π E_{n}}{H}) . \end{matrix}

(5)

This is equivalent to the rate of ionization in the flat Minkowski spacetime in the presence of the heat bath with temperature

T = H / π

This heat bath temperature is twice the Gibbons-Hawking temperature

T_{GH}

, which is usually ascribed to the cosmological horizon,

T = 2 T_{GH}

. Moreover, the electron trajectory is well inside the horizon, since

r_{n} ≪ r_{H} = 1 / H

, and thus this process has no relation to the Hawking radiation. However, in Section 2.4 we show that the relation between the temperature of ionization and Gibbons Hawking temperature,

T = 2 T_{GH}

, is the property of the de Sitter symmetry.

Since the process of ionization takes place well inside the cosmological horizon, one can use the conventional static metric with the gravitational potential

U (r) = - m H^{2} r^{2} / 2

.[20] Then the bound state decays by quantum tunnelling from the point

r = 0

to the point

r = r_{n}

, at which the electron level

- E_{n}

matches the de Sitter gravitational potential

U (r_{n}) = - m H^{2} r_{n}^{2} / 2

. The radial trajectory

p_{r} (r)

is obtained from the classical equation

\frac{p^{2}}{2 m} - \frac{1}{2} m H^{2} r^{2} = - E_{n} .

(6)

One obtains

\begin{matrix} p_{r} (r) = \sqrt{m^{2} H^{2} r^{2} - 2 m E_{n}}, \end{matrix}

(7)

which again gives Equation (5) for the WKB tunneling rate.

2.2. Decay of Composite Particles in de Sitter Spacetime

The same local temperature

T = H / π

describes the process of the splitting of the composite particle with mass m into two components with the larger total mass,

m \to m_{1} + m_{2} > m

, which is also not allowed in the Minkowski vacuum.[17,26,27,28]

It is instructive to derive the rate of this process using also the semiclassical tunneling picture. For simplicity we consider creation of particles with equal masses,

m_{1} = m_{2} > m / 2

. The trajectory of each of the two particles with mass

m_{1}

moving in the radial direction from the origin at

r = 0

is obtained from equation

E (p_{r}, r) = \sqrt{p_{r}^{2} + m_{1}^{2}} + p_{r} H r = \frac{m}{2} .

(8)

We took into account that each of the two particles carries the one half of the energy of the original particle, i.e.

E = m / 2

. The momentum along the trajectory is

p_{r} (r) = \frac{1}{1 - H^{2} r^{2}} [- \frac{m}{2} H r + \sqrt{\frac{m^{2}}{4} - m_{1}^{2} + m_{1}^{2} H^{2} r^{2}}] .

(9)

This momentum is imaginary in the classically forbidden region

r < r_{0}

, where

r_{0} = \sqrt{1 - m^{2} / 4 m_{1}^{2}} / H

. This gives the imaginary contribution to the action:

Im S = Im \int d r p_{r} (r) = \frac{m_{1}}{H} \int_{0}^{r_{0}} d r \frac{\sqrt{r_{0}^{2} - r^{2}}}{r_{H}^{2} - r^{2}} = \frac{π}{4} (2 m_{1} - m) .

(10)

where as before

r_{H} = 1 / H

is the position of the de Sitter horizon. We must take into account that due to momentum conservation, the two particles tunnel simultaneously in the opposite directions. Such coherent process of co-tunneling adds extra factor two in the exponent. As a result one obtains the decay rate of the composite particle into two particles, which is again governed by temperature temperature

T = H / π

Γ (1 \to 2) \propto exp (- 4 Im S) = exp (- \frac{π (2 m_{1} - m)}{H}) .

(11)

In general case, when

m_{2} \neq m_{1}

, the rate of the decay of the composite particle in the limit

m ≫ H

is determined by the same temperature:

Γ (1 \to 2) \sim exp (- \frac{π (m_{1} + m_{2} - m)}{H}) = exp (- \frac{m_{1} + m_{2} - m}{T}) .

(12)

2.3. Triplication of Particles in de Sitter Spacetime

In the same way, massive fermions can be reproduced in the de Sitter environment. For example, the electron at

r = 0

can create the pair – electron and positron which move in the opposite directions. In this process the fermion is triplicated with the rate given by:

Γ (1 \to 3) \sim exp (- \frac{π (3 m - m)}{H}) = exp (- \frac{2 m}{T}) .

(13)

Since the created electron and positron move in the opposite directions, they are detected by two different detectors. Each of the two detectors can detect only single particle, and thus for each detector the radiation rate looks as thermal with the Gibbons-Hawking temperature

T_{GH} = T / 2

Γ (1 \to 3) \sim exp (- \frac{2 m}{T}) = exp (- \frac{m}{T / 2}) = exp (- \frac{m}{T_{GH}}) .

(14)

However, in this process two particles are created simultaneously and coherently (the so-called co-tunneling process). That is why the temperature, which describes such co-tunneling process of radiation of the pair, is twice the Gibbons-Hawking temperature. The same connection between the local temperature and the temperature of the Hawking radiation from the cosmological horizon is discussed in Section 2.4.

It is important that each of three particles (the original electron + electron-positron pair, which is created in the process in Equation (13)) is able to create the other three particles, and then the triplication process continues further. After n replications there will be

3^{n}

fermions (

(3^{n} + 1) / 2

electrons and

(3^{n} - 1) / 2

positrons. Such creation of multiple particles from a single particle immersed in the de Sitter environment demonstrates that the de Sitter vacuum is unstable towards the creation of matter. The consequence of such instability will be discussed in Section 6.

The similar processes take place in the so-called Cosmological Collider,[21,22] where the new particle created by the Hawking radiation plays the role of the external object which produces the heavy particles. In this case we have two different physical processes: the Hawking radiation from the cosmological horizon, and the further local process – the splitting of the created particles, which is determined by the local temperature.

2.4. Connection between the Local and Hawking Temperatures

The local temperature

T = H / π

also determines the process of the Hawking radiation from the cosmological horizon and the Gibbons-Hawking temperature

T_{GH} = T / 2 = H / 2 π

. The reason is that in the Hawking process, two particles are coherently created (the analog of cotunneling): one particle is created inside the horizon, while its partner is simultaneously created outside the horizon.[29] The rate of the coherent cotunneling of two particles, each with energy E, is

w \propto exp (- \frac{2 E}{T})

. However, the observer who uses the Unruh-DeWitt detector can detect only the particle created inside the horizon. For this observer the creation rate

w \propto exp (- \frac{2 E}{T})

is perceived as

w \propto exp (- \frac{E}{T / 2}) = exp (- \frac{E}{T_{GH}}),

(15)

with the Gibbons-Hawking temperature

T_{GH} = T / 2 = H / 2 π

The similar scenario of doubling the Hawking temperature was considered for the black hole horizon. [30,31] In this case the partner of the created particle is in the mirror image of the space-time which replaces the coordinate singularity. Although the existence of such quantum clone of the black hole is problematic, the consideration of the coherent creation of two partners on the two sides of the cosmological horizon is applicable to the de Sitter vacuum.

On the contrary, in the local process of the decay of the atom, which is not related to the cosmological horizon, only single particle (electron) is radiated from the atom. This process is fully determined by the local temperature,

w \propto exp (- \frac{ϵ_{0}}{T})

2.5. Two Detectors: Exited Atom vs Ionized Atom

Note the main difference between the temperature measured by the observer using the Unruh-DeWitt detector (see e.g. Ref.[32] and references therein) and the temperature measured by the observer using ionization of an atom. The ionization process is possible, because the radiated electron moves far away from the atom to position

r = r_{0}

, where its negative gravitational energy compensates the ionization potential. In the Unruh-DeWitt detector, which corresponds to the two-level atom interacting with a quantum field, the electron in the atom is excited but remains in the same position in the same atom. That is why such excitation of electron may only come either by the Hawking radiation, or by radiation of photons, see Section 2.6.

However, in the de Sitter case there is no difference in temperatures measured by two detectors. If in the Unruh-DeWitt detector experiments the Hawking temperature is properly interpreted according to Equation (15), the measured temperature of the Hawking radiation is also

T = 2 T_{GH}

. So, in spite of different physical principles, both detectors in the de Sitter environment show the same physical temperature,

T = 2 T_{GH}

. This also demonstrates the uniqueness of the de Sitter state with its symmetry under generalized translations.

2.6. Radiation of Photons by Atom in de Sitter Environment

Instead of the radiation of electron from the atom, one can consider the radiation of photon by the same atom. In both cases the escape of photon or electron from the atom provides the negative gravitational energy. That is why these processes, which are prohibited in the Minkowski spacetime, are energetically possible in the de Sitter environment. Let us consider the atom in the excited state with energy

E_{0} + ϵ

, where

E_{0}

is the ground state energy. In the de Sitter environment, the radiation of photon is possible even if its energy

c p

exceeds the energy difference between the excited and the ground state level, i.e. when

c p > ϵ

For the relativistic photon the energy conservation equation (3) takes the form (here we use

c = 1

\begin{matrix} \sqrt{p_{r}^{2} + p_{⊥}^{2}} + p_{r} H r = ϵ . \end{matrix}

(16)

This gives the following trajectory of photon:

\begin{matrix} p_{r} (r) = \frac{1}{1 - H^{2} r^{2}} [- ϵ H r \pm \sqrt{ϵ^{2} + p_{⊥}^{2} (H^{2} r^{2} - 1)}] . \end{matrix}

(17)

For

c p_{⊥} > ϵ

, the integration over the classically forbidden region,

r < r_{0}

, where

H^{2} r_{0}^{2} = 1 - ϵ^{2} / p_{⊥}^{2}

, gives the following radiation rate of photon by excited atom:

w \sim exp (- 2 Im S) = exp (- \frac{π (c p_{⊥} - ϵ)}{H}), c p_{⊥} > ϵ .

(18)

Since

r_{0} < 1 / H

, the trajectory of photon in this process is inside the cosmological horizon, and the radiation rate is again determined by the local temperature

T = H / π

Equation (18) demonstrates, that radiation takes place even if the atom is in the ground state, i.e. when

ϵ \to 0

. In this case Equation (18) describes the process of radiation of a single photon in the de Sitter environment:

w \sim exp (- \frac{c p}{T}), T = \frac{H}{π} .

(19)

In this process, the atom in its ground state serves as an external object, which violates the de Sitter symmetry and thus provides the nonzero matrix element for the radiation of photon. This process is certainly different from the Hawking process of radiation.

2.7. Accelerating Detector: Is There Connection between the Local Process and Unruh Radiation?

In the same way as in Section 2.5 and Section 2.6, one may consider different independent processes related to the accelerating detector. One of them is the Unruh radiation measured by the Unruh-DeWitt detector, which could be linked to the apparent event horizon in the Rindler spacetime and to the corresponding Unruh temperature

T_{U} = a / 2 π

, where a is acceleration.[33,34,35] The other processes, such as the local process of ionization of the accelerating atom,[36] have no relation to the Rindler horizon.

Let us consider the process of ionization of an atom moving with acceleration. Similar to Equation (6), the trajectory

p_{x} (x)

of the radiated electron is obtained from the classical equation

\frac{p^{2}}{2 m} - m a x = - ϵ .

(20)

Here we used the equivalence between the acceleration of the reference frame and the constant gravitational field,

g = a

In the WKB approximation and in the limit of slow acceleration,

a ≪ ϵ ≪ m

, the classically forbidden trajectory of electron escaping from the atom gives the following radiation rate:[36]

w \sim exp (- \frac{4 \sqrt{2}}{3} \frac{ϵ}{a} {(\frac{ϵ}{m})}^{1 / 2}) .

(21)

In principle, one can introduce the effective temperature, which is similar to the effective temperature

T_{eff} \sim E l

of hopping electrons in a strong electric field E, where l is the localization length.[37,38] In our case, the analog of the localization length is

l = 1 / \sqrt{m ϵ}

. But otherwise the local process of ionization of the accelerated atom is certainly non-thermal. Since

ϵ ≪ m

, the rate of ionization in Equation (21) essentially exceeds the ionization rate in any thermal process, which involves acceleration,

w_{thermal} \sim exp (- γ ϵ / a)

. This is very different from the ionization of the atom in the de Sitter environment, which looks thermal.

With the same approach one can also calculate the Unruh radiation of photons using different arrangements of detectors. The state of the art in theoretical understanding of Unruh radiation can be found in Refs. [39,40,41] and references therein. Our examples demonstrate that the rate of Unruh radiation depends on details of the considered processes and it is not necessarily thermal. Thermal behavior of the local and global processes in the de Sitter environment is the result of the special de Sitter symmetry.

3. Thermodynamics of the de Sitter State

3.1. De Sitter Symmetry and de Sitter Heat Bath

As distinct from the Unruh effect, different arrangements of detectors in the de Sitter environment show the same temperature. This demonstrates the uniqueness of the de Sitter spacetime in producing the thermal bath with local temperature. The reason for that is that the de Sitter spacetime is homogeneous under the combination of translation and the proper conformal transformations.[42,43] In the PG metric it is the invariance of the de Sitter state under the modified translations,

r \to r - e^{H t} a

, which for

H \to 0

corresponds to the conventional invariance under translations

r \to r - a

in Minkowski spacetime. Due to this combined translational symmetry, all the comoving observers at any point of the de Sitter space observe the same temperature,

T = H / π

. That is why one may conclude, that the de Sitter state is the heat bath produced by gravity.

The uniqueness of the de Sitter thermal state lies in the fact that its temperature does not violate the de Sitter symmetry, and thus does not require the preferred reference frame. This is distinct from thermal state of matter, which always has a preferred reference frame where matter is at rest. As a result, thermal matter violates the de Sitter symmetry, which leads to the heat exchange between the two thermal subsystems, gravity and matter, and finally to the de Sitter decay.

3.2. From Local Temperature to Local Entropy

The gravity subsystem – de Sitter quantum vacuum – has its own temperature and entropy, see also Ref.[44]. On the other hand the de Sitter spacetime serves as the thermal bath for matter. Then the quasi-equilibrium states of the expanding Universe can be described by two different temperatures: the temperature of the gravitational vacuum (temperature of dark energy) and the temperature of the matter degrees of freedom.[45] In this section we discuss the pure de Sitter vacuum without the excited matter ignoring for the moment the thermally activated creation of matter from the vacuum. The excitation and thermalization of matter by the de Sitter thermal bath will be discussed in Section 6.

If the vacuum thermodynamics is determined by the local activation temperature

T = H / π

, then in the Einstein gravity with cosmological constant the vacuum energy density is quadratic in temperature:

ϵ_{vac} = \frac{3}{8 π G} H^{2} = \frac{3 π}{8 G} T^{2} .

(22)

This leads to the free energy density of the de Sitter vacuum,

F = ϵ_{vac} - T s_{vac}

, which is also quadratic in T, and thus the entropy density

s_{vac}

in the de Sitter vacuum is linear in T:

s_{vac} = - \frac{\partial F}{\partial T} = \frac{3 π}{4 G} T = 12 π^{2} K T .

(23)

Here

K = 1 / 16 π G

is the gravitational coupling.

The temperature T and the entropy density

s_{vac}

are the local quantities which can be measured by the local static observer.

3.3. De Sitter Vacuum, Fermi Liquid and Cosmological Constant Problem

The equation (23) demonstrates that the thermal properties of the de Sitter state are similar to that of the non-relativistic Fermi liquid, where the entropy density is also linear in temperature:

s_{FL} = \frac{p_{F}^{2}}{3 v_{F}} T .

(24)

The Fermi velocity

v_{F}

and Fermi momentum

p_{F}

of this cosmological analog of the Fermi liquid are on the order of the speed of light and the inverse Planck length correspondingly,

v_{F} \sim c

and

p_{F} \sim M_{Pl} = 1 / l_{Pl}

. Of course, this is only the parallel, and one should not identify the de Sitter vacuum with the real Fermi liquid. However, the real Fermi surface may form inside the black hole horizon.[46,47]

Since the thermodynamics of the de Sitter state with the thermal energy

ϵ_{vac} \propto T^{2}

is similar to the thermodynamics of the Fermi liquid, let us try to exploit this connection. One of the directions is the Sommerfeld law in Fermi liquid, which states that the entropy per one atom of the Fermi liquid is

S = \frac{s_{FL}}{n_{FL}} \sim \frac{T}{E_{F}},

(25)

where

n_{FL} \sim p_{F}^{3}

is the density of atoms in the Fermi liquid and

E_{F}

is Fermi energy.

We do not know what are the "atoms of the vacuum", but from Equation (23) it follows that the entropy density of the vacuum

s_{vac} \sim T / l_{Pl}^{2} \sim (T / M_{Pl}) / l_{Pl}^{3}

, where

l_{Pl}

is the Planck length and

M_{Pl}

is the Planck energy. This suggests that the density of the "atoms of the vacuum" is

n_{Pl} \sim 1 / l_{Pl}^{3}

and entropy per "atom of the vacuum" is:

S = \frac{s_{vac}}{n_{Pl}} \sim s_{vac} l_{Pl}^{3} \sim \frac{T}{M_{Pl}} .

(26)

Equation (26) is the full analog of the Sommerfeld law for Fermi liquid. This analogy also suggests that the corresponding density of states in the quantum vacuum (the analog of density of states at the Fermi level

N_{F} \sim m p_{F}

in Fermi liquids) is

N_{Pl} \sim M_{Pl}^{2}

. For bosonic and fermionic degrees of freedom of this quantum vacuum the density of states is

N_{Pl} = 9 / 4 π G

and

N_{Pl} = 9 / 2 π G

correspondingly, which can be compared with the value

N_{Pl} = 3 π / G

suggested in Ref. [48]. This huge density of states leads to a very large entropy of the de Sitter state even for very small temperature of the vacuum.

So, the quantum vacuum looks as some specific form of the relativistic Fermi liquid. However, some consequences are the same as in the non-relativistic Fermi liquid. In particular, in the full equilibrium at

T = 0

and in the absence of external pressure,

P = 0

, the energy density of the non-relativistic Fermi liquid is exactly zero,

ϵ (n) - μ n = T s - P = 0

. This follows solely from thermodynamics, and is valid for the macroscopic system in its ground state. In all such systems, the contribution of the zero-point energies of collective modes (phonons, fermionic quasiparticles, magnions, etc.) is exactly compensated by the microscopic (atomic) degrees of freedom. This thermodynamic property does not depend on the microscopic physics, and is easily checked in condensed matter systems, where we know both the micro and macro physics. That is why it is not surprizing, that for the relativistic quantum vacuum, the vacuum energy density is zero, if there is the full thermodynamic equilibrium, the temperature

T = 0

, there is no matter and no external pressure,

ϵ_{vac} (H = 0, T = 0) = - P_{vac} = 0

. The thermodynamics, which is insensitive to the microscopic structure of the vacuum (ground state) solves the main cosmological constant problem. The other cosmological constant problems are discussed in Section 6.6.

3.4. Hubble Volume Entropy vs Entropy of the Cosmological Horizon

Using the entropy density in Equation (23), one may find the total entropy of the Hubble volume

V_{H}

– the volume surrounded by the cosmological horizon with radius

R = 1 / H

S_{bulk} = s_{vac} V_{H} = \frac{4 π R^{3}}{3} s_{vac} = \frac{π}{G H^{2}} = \frac{A}{4 G} = S_{hor},

(27)

where A is the horizon area.

The Hubble-volume entropy coincides with the entropy of the cosmological horizon suggested by Gibbons and Hawking. However, in our approach the thermodynamic entropy comes from the local entropy of the de Sitter quantum vacuum, rather than from the horizon degrees of freedom. It is typically assumed that the horizon microstates are concentrated in the region of the Planck length

l_{Pl} = 1 / M_{Pl}

in the vicinity of horizon, and this leads to the area law for the total entropy inside the horizon.[49] The local thermodynamics leads to the same area law, but without assumptions on the spatial distribution of the degrees of freedom.

The connection between the bulk entropy of the region inside the horizon due to the local vacuum thermodynamics and the surface entropy of the horizon may have the holographic origin, when the horizon is considered as null surface.[49] This may be the reason why the presence of the horizon allows to know the total entropy of the Hubble volume without knowledge on the distribution of the local entropy inside the horizon.

However, the bulk-surface correspondence in Equation (27) is valid only in the (

3 + 1

)-dimension. In the general

d + 1

dimension of spacetime, the same approach gives the factor

(d - 1) / 2

in the relation between the entropy of the Hubble volume and the Gibbons-Hawking entropy of the cosmological horizon,

S_{bulk} = \frac{d - 1}{2} S_{hor}

. This may add to the peculiarities of the

d = 3

space dimension,[50] where in particular the mass dimension of the gravitational coupling,

[K] = d - 1

, coincides with the mass dimension of curvature,

[R] = 2

. The same concerns such pair of thermodynamically conjugate variables as electric field with the mass dimension

[E] = 2

and the electric induction with mass dimension

[D] = d - 1

. Their dimensions also coincide only for

d = 3

. Discussion of the natural dimensions of physical quantities in

d = 3

can be found in Ref. [51].

4. Thermodynamics from the Heat Transfer in the Multi-Metric Gravity Ensemble

4.1. Multi-Metric Gravity

Since the heat exchange between the bodies or between the systems is the main source of the emergent thermodynamics,[52] we can consider the de Sitter thermodynamics from the point of view of the heat transfer between different cosmological objects.

Such heat exchange can be discussed in the frame of the so-called multi-metric gravity, see Ref.[53] and references therein. The corresponding model action of the whole system can be written as the sum of actions of the sub-systems in the same coordinate spacetime:

S = - \int d^{4} x \sum_{n = 1}^{N} L_{n}, L_{n} = \sqrt{- g_{(n)}} (K_{n} R {g_{μ ν (n)}} + Λ_{n}) .

(28)

Then the Universe can be seen as the system of N sub-Universes, each with its own gravitational coupling

K_{n}

, cosmological constant

Λ_{n}

and metric

g_{μ ν (n)}

Following Frogatt and Nielsen[54] one can introduce N independent tetrad fields

e_{μ}^{a (n)}

for N fermionic species. In this multi-tetrad gravity one has the ensemble of the gravitational and cosmological constant actions:

\begin{matrix} L_{n} = e_{a b c d} K_{n} R^{a b (n)} \land e^{c (n)} \land e^{d (n)} + \\ + e_{a b c d} Λ_{n} e^{a (n)} \land e^{b (n)} \land e^{c (n)} \land e^{d (n)} . \end{matrix}

(29)

And the corresponding ensemble of actions for the fermionic species:

S_{M} = e_{a b c d} \int \sum_{n} Θ^{a (n)} \land e^{b (n)} \land e^{c (n)} \land e^{d (n)},

(30)

Θ^{a (n)} = \frac{i}{2} [{\bar{Ψ}}^{(n)} γ^{a} D_{μ} Ψ^{(n)} - D_{μ} {\bar{Ψ}}^{(n)} γ^{a} Ψ^{(n)}] d x^{μ} .

(31)

This can be extended to the multi-fünfbein gravity, where instead of the tetrad fields the Dirac fermions are described by the rectangular vielbein (fünfbein).[55]

On the other hand, gravity with multiple tetrad fields may come from the Akama-Diakonov-Wetterich theory, [56,57,58,59,60,61,62,63,64] where the tetrads are formed as composite objects – the bilinear combinations of the fundamental fermionic fields:

e_{μ}^{a (n)} = 〈Θ^{a (n)}〉 .

(32)

In this approach, the metric is the quartet of fermions. In principle, the so called vestigial gravity can be realized, in which the bilinear combination of fermions in Equation (32) is zero,

e_{μ}^{a (n)} = 0

, while the metric – the quartet of fermions – is nonzero:[65]

g_{μ ν (n)} = η_{a b} 〈Θ_{μ}^{a (n)} Θ_{ν}^{b (n)}〉 .

(33)

4.2. Heat Exchange in Multi-Metric Gravity

The heat exchange between the sub-Universes leads to their equilibration with formation of the common expansion rate and thus the common temperature. We consider first the system of two Universes, assuming that in each of them the entropy of horizon obeys the area law, and show that the maximum entropy corresponds to the state in which both states have the same expansion rate.

In the de Sitter state, which is determined by the cosmological constant, the equation of state for the vacuum energy is

ϵ_{vac} = - P_{vac}

. The total vacuum energy is proportional to the volume V of the system, if we assume that the volume V is much larger than the Hubble volume,

V ≫ V_{H}

, so that the boundary terms are not important. Then we have:

E_{V} = ϵ_{vac} V = 6 K H^{2} V .

(34)

Let us assume that the bulk-surface correspondence is valid, i.e. the entropy of the Hubble volume

V_{H}

is equal to the Gibbons-Hawking entropy of cosmological horizon,

S_{V_{H}} = S_{hor} = 4 π K A

. Then the total entropy

S_{V}

in the volume

V ≫ V_{H}

can be obtained from the entropy of the Hubble volume

V_{H}

S_{V} = S_{hor} \frac{V}{V_{H}} = 12 π K H V .

(35)

Let us now consider two de Sitter sub-states with different values of the gravitational coupling,

K_{1}

and

K_{2}

, and different values of the Hubble parameter,

H_{1}

and

H_{2}

\begin{matrix} S = - \int d^{4} x \sqrt{- g_{(1)}} (K_{1} R {g_{μ ν (1)}} + Λ_{1}) - \\ - \int d^{4} x \sqrt{- g_{(2)}} (K_{2} R {g_{μ ν (2)}} + Λ_{2}) . \end{matrix}

(36)

This corresponds to the higher dimensional analog of the bilayer graphene,[66] where two 2+1 dimensional Universes are in the neighbouring layers of the 3+1 spacetime. In this interpretation we have two 3+1 dimensional Universes in the neighbouring layers in the 4+1 space.

The total energy and total entropy of two layers are (if the interaction between the layers is neglected):

E_{V} = E_{1} + E_{2} = 6 (K_{1} H_{1}^{2} + K_{2} H_{2}^{2}) V,

(37)

S_{V} = S_{1} + S_{2} = 12 π (K_{1} H_{1} + K_{2} H_{2}) V .

(38)

Let us now allow for the energy exchange (the heat exchange) between these two Universes (analogs of the two layers of graphene). This exchange can be realized by the matter field, which interacts with both metrics. It leads to the variations of the Hubble parameters

H_{1}

and

H_{2}

at fixed

E_{V}

. If we ignore the thermalization of matter by de Sitter environment, the heat exchange will finally produce the equilibrium state with the maximum entropy S, in which the Hubble parameters become equal:

H_{1}^{2} = H_{2}^{2} = \frac{E_{V}}{6 (K_{1} + K_{2}) V} \equiv H^{2} .

(39)

The equilibration of the Hubble parameters demonstrates that the Hubble parameter (with some numerical factor) plays the role of the temperature of the de Sitter Universe.

The temperature of the de Sitter Universe can be obtained by variation over the Hubble parameter:

\begin{matrix} \frac{1}{T_{1}} = \frac{d S_{1}}{d E_{1}} = \frac{d S_{1} / d H_{1}}{d E_{1} / d H_{1}} = \frac{π}{H_{1}}, \\ \frac{1}{T_{2}} = \frac{d S_{2}}{d E_{2}} = \frac{d S_{2} / d H_{2}}{d E_{2} / d H_{2}} = \frac{π}{H_{2}}, \end{matrix}

(40)

with

T_{1} = T_{2} = H / π

in equilibrium.

In case of the arbitrary number N of the sub-Universes, the heat exchange between them leads to the state of the Universe in which all the sub-Universes coherently expand with the same rate H, i.e., with the same de Sitter metric in all the subsystems. The whole Universe has the gravitational coupling K equal to the sum of the individual couplings in the sub-Universes and the vacuum energy density equal to the sum of energy densities of subsystems:

E_{V} = 6 K H^{2} V, K = \sum_{n} K_{n}, Λ = \sum_{n} Λ_{n},

(41)

with

T_{n} = T = H / π

4.3. Thermodynamics from the Multi-Metric Ensemble

Let us remind that in the above approach we used the bulk-horizon correspondence

S_{V_{H}} = S_{hor} = 4 π K A

, which finally leads to the equilibrium Universe with temperature

T = H / π

. Let us now consider the thermodynamics of the whole de Sitter system without assumption about the entropy of the cosmological horizon. For that we consider the statistical ensemble of N de Sitter sub-Universes with random Hubble parameters

H_{n}

. This is the extension of the multi-metric gravity to the statistical ensemble with the randomly distributed parameters

K_{n}

and

Λ_{n}

For large N, the random distribution of the parameters results in the exponential behaviour of the distribution functions,

w_{n} \propto exp (- E_{n} / T)

, with the same parameter T for all subsystems. As in the statistical ensemble of atoms, where the temperature of the system is determined by the physical processes, the temperature of the ensemble of the sub-Universes factor is also determined by the physical processes. In our case it is the of the behaviour of matter (atom) in the de Sitter environment, which gives

T = H / π

. This connection between T and H is rather natural. Both, the parameter T, which plays the role of temperature, and the Hubble parameter H are the quantities which in equilibrium become common for all the subsystems in the ensemble, and they have the same dimension of inverse time,

[T] = [H] = [1 / t]

The physical temperature in turn gives rise to the total entropy and to the local entropy,

S_{V} = \sum_{n} S_{n} = 12 π K H V = s_{loc} V

. So, in this scenario the de Sitter entropy comes from a set of many randomly distributed subsystems with the expansion rates

H_{n}

. Due to the heat exchange at fixed total energy

E_{V}

these states are organized in the equilibrium thermal state, which corresponds to the coherent de Sitter expansion of the whole system. The coherence due to thermalization may explain the horizon problem, i.e. why the causally-disconnected regions of the CMB are in thermal equilibrium.

4.4. Regularization vs Thermalization

The multi-metric ensemble may include the ensemble of N species of Weyl or Dirac fermions. At large N, all tetrads in the random ensemble approach the same value,

e_{μ}^{a (n)} \to e_{μ}^{a}

, and thus in the equilibrium state all fermionic species experience the same geometry. In Refs. [54,67] the formation of the common Lorentz invariance for different fermionic species is also considered. But this is achieved by the renormalization group effect in the infrared limit, instead of thermalization. This suggests the possible connection between renormalization and thermalization.

One may expect that the heat exchange between subsystems leads not only to the coherence of the de Sitter states, but to the general coherence of the metric fields, when the metric fields

g_{μ ν (n)}

of the subsystems become equal, thus forming the common metric

g_{μ ν}

. If this is true, this could be some kind of the thermodynamic gravity, but without using the holographic principle.

4.5. Coherence vs Thermalization

At first glance this formation of the coherently expanding state from the ensemble of the microstates looks similar to the formation of the coherent spin precession (magnon BEC) from the incoherent precessions about the local magnetic fields with random frequencies

ω_{n}

.[68] These random frequencies correspond to the random Hubble parameters

H_{n}

in different sub-Universes. The coherence of precession develops due to the spin currents between the regions of the local precessions – the analog of the heat exchange between the sub-Universes. The formed common frequency

ω

of the coherent precession corresponds to the formed common Hubble parameter H of the large Universe. Moreover, they have the same dimension of the inverse time,

[H] = [ω] = [1 / t]

, while the dimensionless magnon number (or the spin projection

S_{z}

) corresponds to the entropy which is also dimensionless.

However, the source of the coherence is the exchange of spin instead of the exchange of the energies. As a result the formation of the coherent state of spin precession is due to minimization of the total energy E at fixed projection

S_{z}

of the total spin on magnetic field. This leads to the common frequency, which plays the role of the chemical potential

μ

for magnons, which emerges due to the exchange of quasiparticles (magnons) between the regions. That is why this process is quite opposite to the formation of the common temperature, where the total energy is fixed, while entropy reaches its maximum value.

Anyway, in all the cases the parameters, which are the same in all subsystems in equilibrium – common frequency

ω

, common chemical potential

μ

, common temperature T, common angular velocity

Ω

and now also the common Hubble parameter H – all of them have the same dimension of inverse time,

[T] = [H] = [μ] = [ω] = [Ω] = [1 / t]

. In Section 4.6 it is shown that the Hubble parameter H as the thermodynamic quantity enters the chiral anomaly effects together with the conventional variables T,

μ

and

Ω

4.6. De Sitter Contribution to Chiral Anomaly

As the thermodynamic quantity, the Hubble parameter H participates in different thermodynamical effects. We consider this on example of the chiral vortical effect – the appearance of the chiral current in fermionic systems in the presence of rotation. For Dirac fermions in the flat spacetime, the chiral current

j_{A}

contains the following contributions:[69,70,71,72,73]

j_{A} = (\frac{T^{2}}{6} + \frac{μ^{2}}{2 π^{2}} + \frac{Ω^{2}}{24 π^{2}}) Ω .

(42)

In the de Sitter state the gravitational thermodynamical variable – the curvature

R

– is added.[74,75] According to Ref. [75] the gradient expansion gives the following contribution to the chiral current, which is very similar to the contributions of other thermodynamic quantities in Equation (42):

j_{A} = \frac{H^{2}}{8 π^{2}} Ω .

(43)

The same term is obtained for the anti-de Sitter spacetime where

H^{2} < 0

.[76] Also, in Ref.[74] the curvature term comes from the shift of the fermionic mass gap due to curvature,

- M^{2} \to - (M^{2} + H^{2})

, and this leads to the Equation (43) with opposite sign.

Comparison of Equation (43) with Equation (42) demonstrates that there is the difference between the contribution

T^{2} / 6

in Equation (42), which comes from the temperature of matter, and the contribution

T^{2} / 8

from the temperature

T = H / π

of the de Sitter environment in Equation (43). However, it is possible that the more rigorous calculations (beyond the gradient expansion, with the proper conservation laws and with the proper limit cases) can modify the coefficient in Equation (43). It is not excluded that these two contributions may cancel each other when the matter and the gravitational background are in equilibrium and thus have the same temperature. Such cancellation of the currents generated by two different mixed gravitational anomalies in rotating chiral liquid under the full equilibrium was found in Ref. [77]. This supports the Bloch theorem on the absence of the total current in equilibrium, see also Refs. [78,79,80].

Anyway, the participation of the curvature

R = - 12 H^{2}

in the thermodynamics of the chiral anomaly demonstrates the uniqueness of the de Sitter state in providing the contributions of gravitational variables to different thermodynamic effects together with the traditional thermodynamic variables, such as temperature, chemical potential, angular velocity, electric and magnetic fields.

5. Thermodynamics of de Sitter State and $f (R)$ Gravity

5.1. Thermodynamic variables in $f (R)$ gravity

Here we consider the thermodynamics of the de Sitter state in terms of the gravitational variables and the corresponding modification of the thermodynamic Gibbs-Duhem relation for the quantum vacuum.

The conventional vacuum pressure

P_{vac}

obeys the equation of state

w = - 1

and enters the energy momentum tensor of the vacuum medium in the form:

T^{μ ν} = Λ g^{μ ν} = diag (ϵ_{vac}, P_{vac}, P_{vac}, P_{vac}), P_{vac} = - ϵ_{vac} .

(44)

In the de Sitter state the vacuum pressure is negative,

P_{vac} = - ϵ_{vac} < 0

Due to the linear dependence of the de Sitter entropy density on temperature this pressure

P_{vac}

does not satisfy the standard thermodynamic Gibbs-Duhem relation,

T s_{vac} = ϵ_{vac} + P_{vac}

, because the right hand side of this equation is zero. The reason for that is that in this equation we did not take into account the gravitational degrees of freedom of quantum vacuum. Earlier it was shown, that gravity contributes with the pair of the thermodynamically conjugate variables: the gravitational coupling

K = \frac{1}{16 π G}

and the scalar Riemann curvature

R

, see Refs.[9,81,82]. The contribution of the term

K R

to thermodynamics is similar to the work density.[83,84,85,86]

The quantities K and

R

can be considered as the local thermodynamic variables, which in condensed matter physics are similar to temperature, pressure, chemical potential, number density, spin density, etc. Indeed, since the de Sitter spacetime is maximally symmetric, its local structure is characterized by the scalar curvature alone, while all the other components of the Riemann curvature tensor are expressed via

R

R_{μ ν α β} = \frac{1}{12} (g_{μ α} g_{ν β} - g_{μ β} g_{ν α}) R .

(45)

That is why the scalar Riemann curvature as the covariant quantity naturally serves as one of the thermodynamical characteristics of the macroscopic matter.[87,88]

Another argument is related to the so-called Larkin-Pikin effect.[89] This is the jump in the number of degrees of freedom, when the fully homogeneous state is considered. One has the extra parameters, which are space independent, but participate in thermodynamics. [90,91,92] The same concerns the constant electric and magnetic fields in vacuo, which together add three more degrees of freedom. These constant fields are mutually independent, in contrast to the spacetime-dependent fields connected by the Maxwell equations.[92] The scalar curvature

R

in the de Sitter vacuum, which is constant in space-time, also serves as such thermodynamic parameter. Then the gravitational coupling

K = d f / d R

serves as the analog of the chemical potential, which is constant in the full equilibrium.

5.2. Gibbs-Duhem Relation in $f (R)$ Gravity

The new thermodynamic variables, K and

R

, which come from the gravity, and Eq. (23) for the entropy density allow us to restore the Gibbs-Duhem relation for de Sitter vacuum in the following form:

T s_{vac} = ϵ_{vac} + P_{vac} - K R .

(46)

This equation is obeyed, as can be checked on example of the Einstein gravity, where

T s_{vac} = 12 π^{2} K T^{2} = 12 K H^{2}

, using the equations

ϵ_{vac} + P_{vac} = 0

and

R = - 12 H^{2}

. This supports the earlier proposal that K and

R

can be considered as the thermodynamically conjugate variables.[81,82]

The Equation (46) can be also written using the effective vacuum pressure, which absorbs the gravitational degrees of freedom:

P = P_{vac} - K R .

(47)

Then the conventional Gibbs-Duhem relation is restored:

T s_{vac} = ϵ_{vac} + P .

(48)

The equation (48) is just another form of writing the Gibbs-Duhem relation (46). But it allows to make different interpretation of the de Sitter vacuum state. The introduced effective de Sitter pressure P is positive,

P = ϵ_{vac} > 0

, and satisfies equation of state

w = 1

, which is similar to matter with the same equation of state. As a result, due to the gravitational degrees of freedom, the de Sitter state has many common properties with the non-relativistic Fermi liquid, where the thermal energy is proportional to

T^{2}

, and also with the relativistic stiff matter with

w = 1

introduced by Zel’dovich.[93]

5.3. Entropy of Cosmological Horizon in Terms of Effective Gravitational Coupling

Let us now show that the holographic bulk-surface correspondence remains valid also in the

f (R)

gravity, i.e. that the entropy of the Hubble volume coincides with the entropy of the cosmological horizon,

S_{hor} = 4 π K A

In the

f (R)

gravity the action is:

S = - \int d^{4} x \sqrt{- g} f (R) .

(49)

In the equilibrium de Sitter state the curvature is determined by the Einstein equations obtained by variation of the action (49):

2 f (R) = R \frac{d f}{d R} .

(50)

This gives the following generalization of the vacuum energy density and Gibbs-Duhem relation for the de Sitter states (i.e. for the states with constant four-dimensional curvature) in the

f (R)

gravity:

\begin{matrix} ϵ_{vac} = f (R) - K R, K = \frac{d f}{d R} . \end{matrix}

(51)

\begin{matrix} T s_{vac} = ϵ_{vac} + P_{vac} - K R = - K R, \end{matrix}

(52)

Here K is the natural definition of the variable, which is thermodynamically conjugate to the curvature

R

, while

ϵ_{vac}

serves as the corresponding thermodynamic potential.

Now we use the fact, that the local temperature

T = H / π

of the equilibrium de Sitter state is the geometric property of the de Sitter. It is determined by the PG metric, which regulates the process of the ionization of the atom in the de Sitter environment, and thus it does not depend on the function

f (R)

. Using this local temperature one obtains the local entropy

s_{vac}

from Equation ():

s_{vac} = - K R / T

, where

R = - 12 H^{2} = - 12 π^{2} T^{2}

. Then the total entropy of the Hubble volume

V_{H}

is given by the same Equation (27) as in the Einstein gravity:

S_{bulk} = s_{vac} V_{H} = 4 π K A = S_{hor} .

(53)

But now K is the effective gravitational coupling in Equation (51).

This generalization of the Gibbons-Hawking entropy was discussed in Refs.[9,94,95,96]. But here it was obtained using the local thermodynamics of the de Sitter vacuum. This demonstrates that the local thermodynamics of the de Sitter vacuum is valid also for the

f (R)

gravity. The effective gravitational coupling K serves as one of the thermodynamic variable of the local thermodynamics. This quantity plays the role of the chemical potential, which is thermodynamically conjugate to the curvature

R

, and it is constant in the thermodynamic equilibrium state of de Sitter spacetime.

5.4. Example of Quadratic Gravity

For illustration, we consider the simple example of the

f (R)

gravity and the corresponding modification of the gravitational coupling K in the de Sitter environment. In the conventional Einstein gravity, where

f (R) = K_{0} R + Λ

, the de Sitter state has the equilibrium value of the curvature,

R_{0} = - 2 Λ / K_{0} = - 12 H^{2}

. Let us add the quadratic term to the Einstein action:[9,94]

f (R) = K_{0} R - \frac{1}{2} ϵ_{G} R^{2} + Λ .

(54)

Here

ϵ_{G}

is the dimensionless parameter. In electrodynamics such parameter corresponds to such parameters as dielectric constant, magnetic permeability and inverse fine structure constant. These parameters contain the logarithm,

ln \frac{M_{Pl}^{4}}{B^{2}}

, with the prefactor depending on the massless fermionic and bosonic fields. In gravity, there are also the logarithmic corrections,

ln \frac{M_{Pl}^{4}}{R^{2}}

, but here we ignore these contributions.

In this analogy with electrodynamics, the parameter

K_{0}

corresponds to spontaneous magnetization or spontaneous polarization, which break the corresponding discrete symmetries. In our case, it is the symmetry with respect to transformation

R \to - R

, which takes place under the coordinate transformation

x^{μ} \to i x^{μ}

and corresponds to the transition from de Sitter to anti-de Sitter. The complex metric was considered in Ref.[97]. This is different from the time reversal symmetry operation, which connects the black and white holes discussed in Section 8.5, and the expanding and contracting de Sitter states discussed in Section 7.2.

The equilibrium curvature

R_{0}

in the

f (R)

gravity can be obtained from Equation (50):

\begin{matrix} R_{0} = - 2 \frac{Λ}{K_{0}} = - 12 H^{2}, \end{matrix}

(55)

It is the same as in Einstein gravity, because the quadratic terms in Equation (50) are cancelled: The equilibrium value of the effective gravitational coupling K is:

\begin{matrix} K = \frac{d f}{d R} |_{R = R_{0}} = K_{0} + 2 ϵ_{G} \frac{Λ}{K_{0}} . \end{matrix}

(56)

This modified gravitational coupling K determines the local entropy

s_{vac}

, which follows from Equation (). As a result, the entropy of the Hubble volume in Equation (57), which we identify with the entropy of the horizon

S_{hor}

, is also determined by the modified coupling K:

\begin{matrix} S_{hor} = s_{vac} V_{H} = 4 π K A . \end{matrix}

(57)

The local and global entropies change sign for

K < 0

, while the cosmological expansion is still described by the de Sitter metric. However, the negative K requires the negative parameter

ϵ_{G} < 0

, which marks the instability of such de Sitter vacuum.[94]

6. From de Sitter Thermodynamics to de Sitter Decay

6.1. De Sitter State as Thermal Bath for Matter

The validity of the holographic connection between the bulk and surface entropies in the extension of the thermodynamics to the

f (R)

gravity supports the idea that the de Sitter vacuum is the thermal state with the local temperature

T = H / π

. The gravitational temperature, which is twice the Hawking temperature, has been also obtained in the particular de Sitter limit,[98] when the relativistic and non-relativistic matter tend to zero (see the footnote 2 on page 4). This demonstrates that in the conventional approaches to the de Sitter thermodynamics, where the Euclidean time is used, the results may depend on the choice of the order of limits.

The nonzero local temperature of the gravitational vacuum shows that the de Sitter vacuum is locally unstable towards the creation of matter, if some matter (such as atom or electron), is originally present, see Section 2.3. This is distinct from the mechanism of creation of the pairs of particles by Hawking radiation from the cosmological horizon, which may or may not lead to the decay of the vacuum energy. There are still controversies concerning the stability of the de Sitter vacuum caused by the Hawking radiation, see e.g. [91,99,100] and references therein.

6.2. De Sitter Decay due to Thermalization of Matter by de Sitter Heat Bath

To describe the decay of the vacuum due to activation and thermalization of matter, the extension of the Starobinsky analysis of the vacuum decay[101,102,103,104] is needed. Especially the revolutionary stochastic inflation approach pioneered by Starobinsky[105,106] is extremely useful, although it requires some modifications.[107,108,109,110] This also includes the so-called separate universe approach, which is somewhat similar to the multi-metric gravity discussed in Section 4. Here we consider the simple phenomenological scenario based on the energy exchange between the thermal de Sitter and the thermal matter. This phenomenological description does not depend on the details of the microscopic (UV) theory, and requires only the slow-roll condition, i.e. the slow variation of the Hubble parameter,

| \dot{H} | ≪ H^{2}

, or which is the same

| \dot{T} | ≪ T^{2}

The thermal exchange between the de Sitter heat bath and the excited matter generates the thermal relativistic gas. The temperature of relativistic gas tends to approach the temperature

T = H / π

of the de Sitter background. Correspondingly, the energy density of this matter

ϵ_{M}

tends to approach the value

ϵ_{M} \sim T^{4}

. In terms of the Hubble parameter, this is

ϵ_{M} \to b H^{4}

, where the dimensionless parameter b depends on the number of massless relativistic fields. For example,

b = 7 N_{F} / 120 π^{2}

for

N_{F}

species of massless Weyl fermions.

The energy exchange between the vacuum heat bath and matter can be described by the following dynamical modification of the Friedmann equations,[111] where the dissipative Hubble friction equation

\partial_{t} ϵ_{M} = - 4 H ϵ_{M}

is extended to

\begin{matrix} \partial_{t} ϵ_{M} = - 4 H (ϵ_{M} - b H^{4}) . \end{matrix}

(58)

This equation describes the tendency of matter to approach the local temperature of the vacuum,

T = H / π

. The extra gain of the matter energy,

4 b H^{5}

, must be compensated by the corresponding loss of the vacuum energy:

\begin{matrix} \partial_{t} ϵ_{vac} = - 4 b H^{5}, \end{matrix}

(59)

Since the vacuum energy density is

ϵ_{vac} = 6 K H^{2}

, one obtains from Equation (59) the following time dependence of the Hubble parameter and of the energy densities of vacuum and matter:

\begin{matrix} H (t) = b^{- 1 / 3} M_{Pl} {(\frac{t_{Pl}}{t + t_{0}})}^{1 / 3}, \end{matrix}

(60)

\begin{matrix} ϵ_{vac} (t) = 6 b^{- 2 / 3} M_{Pl}^{4} {(\frac{t_{Pl}}{t + t_{0}})}^{2 / 3}, \end{matrix}

(61)

\begin{matrix} ϵ_{M} (t) = b H^{4} = b^{- 1 / 3} M_{Pl}^{4} {(\frac{t_{Pl}}{t + t_{0}})}^{4 / 3} . \end{matrix}

(62)

Here

M_{Pl}

is the Planck mass,

M_{Pl}^{2} = K

, and

t_{Pl} = 1 / M_{Pl}

is Planck time. We assume that

t_{0} ≫ t_{Pl}

, and thus

| \dot{H} | ≪ H^{2}

Thus the thermal character of the de Sitter state determines the process of its decay. The obtained power law decay of H in Equation (60) was also found in Refs. [112,113,114,115,116,117], although using different approaches. In the Padmanabhan model,[112,113] the de Sitter horizon is considered as the photosphere with the Gibbons-Hawking temperature and with the radiative luminosity

d E / d t \propto T^{4} A_{H}

, where

A_{H} = 4 π / H^{2}

is the area of horizon. Since the energy of the Hubble volume is

E \sim M_{Pl}^{2} / H

, and

T^{4} A_{H} \sim H^{2}

, this leads to the power law for the vacuum energy density in Equation (). As was mentioned by Padmanabhan,[113] in his model the late time cosmological constant is independent of its initial value, see Equation () at

t ≫ t_{0}

In Refs. [114,115,116] the Starobinsky stochastic inflation approach has been used. The parameter b therein is proportional to the number N of conformal fields and the parameter

t_{0}

is related to the initial value of the Hubble parameter at the beginning of inflation at

t = 0

H (t = 0) = b^{- 1 / 3} M_{Pl} {(\frac{t_{Pl}}{t_{0}})}^{1 / 3} ≪ M_{Pl} .

(63)

This

H (t = 0)

corresponds to the scaleron mass M in Starobinsky inflation. The time

t_{0} \sim E_{Pl}^{2} / H_{t = 0}^{3}

is called the quantum breaking time of space-times with positive cosmological constant.[118,119]

This demonstrates that the phenomenological scenario of thermalization of matter by the de Sitter heat bath in Eqs. (58) and (59) is rather common. It produces the inflation in terms of two phenomenological parameters, b and

t_{0}

, which determine the decay of the vacuum energy density in Equation (). However, in Section 6.4 we consider another phenomenological approach, which gives different power law for the de Sitter decay.

6.3. Connection to Holographic Principle

The evolution of the gravitational (dark) energy in Eq. () and of the energy of the relativistic matter in Equation () allows us to consider another proposal made by Padmanabhan [120] (see also Refs.[121,122] and references therein). It is the holographic postulate which connects the expansion of the Hubble volume with the difference between the number

N_{hor}

of microstates on the surface of horizon (one degree of freedom per Planck area) and the number

N_{bulk}

of the degrees of freedom in bulk:

\begin{matrix} \frac{d V_{H}}{d t} = G (N_{hor} - N_{bulk}) . \end{matrix}

(64)

This postulate suggests that the expansion of the universe is being driven towards the holographic equipartition, so that in the equilibrium de Sitter state all the bulk degrees of freedom inside the horizon can be expressed via the horizon degrees of freedom,

N_{bulk} = N_{hor}

Instead of the speculative degrees of freedom, we consider here the corresponding thermodynamic entropy. We already found that according to Equation (27) the gravitational entropy of the Hubble volume is equal to the entropy related to horizon,

S_{bulk} = S_{hor}

. Let us consider what happens in the presence of matter. On one hand, matter adds its contribution

S_{M}

to the bulk entropy, and thus

S_{bulk} = S_{M} + S_{hor}

. On the other hand, matter violates the de Sitter symmetry, which leads to the time dependence of the Hubble volume.

The entropy density of matter

s_{M} (t)

can be obtained from the matter energy density in Equation ():

\begin{matrix} s_{M} (t) = \frac{4 π}{3} b H^{3} (t) . \end{matrix}

(65)

Then the total entropy of matter

S_{M}

in the Hubble volume is time independent:

\begin{matrix} S_{M} = s_{M} (t) V_{H} (t) = {(\frac{4 π}{3})}^{2} b . \end{matrix}

(66)

The time derivative of the Hubble volume

d V_{H} / d t

, which is obtained from Equation (60), is also time independent:

\begin{matrix} \frac{d V_{H}}{d t} = \frac{4 π}{3} b M_{Pl}^{2} . \end{matrix}

(67)

Comparing Equation (67) with Equation (66) one has

\begin{matrix} \frac{d V_{H}}{d t} = \frac{3}{4 π} l_{Pl}^{2} S_{M}, \end{matrix}

(68)

and then using equation

S_{M} = S_{bulk} - S_{hor}

one obtains the general relation between the expansion of the Hubble volume and the difference between the bulk entropy and and its holographic surface value:

\begin{matrix} \frac{d V_{H}}{d t} = 12 G (S_{bulk} - S_{hor}) . \end{matrix}

(69)

Up to the sign and numerical coefficient, this coincides with Equation (64), which supports the Padmanabhan holographic conjecture.[120]

6.4. De Sitter Decay and Zel’dovich Stiff Matter

As was mentioned by Padmanabhan, his photosphere model[113] leads to a late time cosmological constant in Equation (), which is independent of the initial value, but its value is still far too large. Can we fix this? In Section 5.2 we obtained that the thermodynamics of de Sitter thermal bath has also the properties of the Zel’dovich stiff matter with

w = 1

. Let us try the stiff matter scenario using our phenomenological approach.

We assume that the dynamics of the decaying de Sitter state can be considered as a kind of two-fluid hydrodynamics – the vacuum component with

w = - 1

, which has de Sitter symmetry, and the stiff matter component with

w = 1

, which violates this symmetry. These two components tend to approach the common temperature. Such two-fluid behaviour of the de Sitter state may also come from the observation in Sec. Ref. Section 6.5 that thermal fluctuations of the energy density in the Hubble volume are on the order of the vacuum energy density itself,

< {(Δ ϵ_{vac})}^{2} > / < ϵ_{vac} >^{2} \sim 1

. So, in this speculations, the de Sitter state behaves as a mixture of dark energy (the de Sitter vacuum) and dark matter (the stiff matter or the thermal fluctuations of de Sitter).

For the (dark) matter with

w = 1

, the dissipative Hubble friction equation is

\partial_{t} ϵ_{DM} = - 6 H ϵ_{DM}

. Due to the energy exchange between the gravitational (dark energy) component and the dark matter component, the temperature of dark matter tends to approach the heat bath temperature

T = H / π

. Then instead of Eqs.(58) and (59) one obtains

\begin{matrix} \partial_{t} ϵ_{DM} = - 6 H (ϵ_{DM} - \tilde{b} H^{2}), \end{matrix}

(70)

and

\begin{matrix} \partial_{t} ϵ_{vac} = - 6 \tilde{b} H^{3} . \end{matrix}

(71)

Here

\tilde{b}

is the phenomenological dimensionless parameter on the order of unity, which microscopic origin is to be found. The similar equations with the corresponding phenomenological dimensionless parameter

γ

were suggested in Ref.[123], where the Polyakov scenario[100] of the infrared instability of the de Sitter space was discussed and the pressureless matter was considered,

w = 0

The Equation (71) gives the following power law decay of dark energy and dark matter:

\begin{matrix} ϵ_{vac} (t) \sim ϵ_{DM} (t) \sim M_{Pl}^{4} {(\frac{t_{Pl}}{t + t_{0}})}^{2} . \end{matrix}

(72)

For large

t ≫ t_{0}

this gives the reasonable order of magnitude of the vacuum energy density and the energy density of matter in the present time:

\begin{matrix} ϵ_{vac} (t_{present}) \sim ϵ_{DM} (t_{present}) \sim \frac{M_{Pl}^{2}}{t_{present}^{2}} \sim 10^{- 120} M_{Pl}^{4} . \end{matrix}

(73)

The same behaviour of the vacuum energy density was obtained using the Hawking 4-form field.[9,124]. In this case the role of dark matter is played by the oscillations of the vacuum energy during its decay.[125] Note that in our approach, both dark energy and dark matter come from the gravitational degrees of freedom. In this sense it has relations to Refs. [126,127,128] and references therein, where the role of the gravitational degrees of freedom is discussed.

6.5. Thermal Fluctuations in de Sitter State

Here we consider thermal fluctuations in the de Sitter thermal state, which also may serve as the source of the two-fluid behaviour of the de Sitter dynamics.

If the de Sitter state represents the excited thermal state of the quantum vacuum, the thermal fluctuations of the deep quantum vacuum may play the role of the dark matter. According to Landau-Lifshitz,[129] the thermal fluctuations are determined by the compressibility of the system and the considered volume V:[124]

〈{(Δ ϵ_{vac})}^{2}〉 = 〈{(Δ P_{vac})}^{2}〉 = \frac{T}{V χ_{vac}} .

(74)

Here

χ_{vac}

is the vacuum compressibility[92] – the compressibility of the fully equilibrium Minkowski vacuum with

ϵ_{vac} = - P_{vac} = 0

Note the main difference between the thermal fluctuations and quantum fluctuations. The contribution of the quantum fluctuations of the relativistic quantum fields to the vacuum energy density is typically on the order of

M_{Pl}^{4}

, where

M_{Pl}

is the Planck mass. But in the fully equilibrium vacuum state this contribution is cancelled by the ultraviolet trans-Planckian degrees of freedom due to the thermodynamic Gibbs-Duhem relation.[92,124] This cancellation is universal, being valid both for the relativistic vacuum states and for the non-relativistic grounds states of the condensed matter systems. On the other hand, the contribution of thermal fluctuations to the vacuum energy is in the range of the infrared physics, which is determined by temperature T and the compressibility of the vacuum.

The vacuum compressibility is not constrained by the thermodynamic laws and is determined by the ultraviolet physics[92] with its Planck energy scale,

χ_{vac}^{- 1} \sim M_{Pl}^{4}

. In this relation it is similar to the gravitational coupling, which is also determined by the Planck scale,

K \sim M_{Pl}^{2}

. On the other hand, the temperature corrections to

χ_{vac}^{- 1}

and K as well as the Casimir corrections are within the range of the infrared physics, see Ref. [130] for the universal temperature correction to the gravitational coupling K. The contribution to the compressibility from the infrared range was discussed in Refs.[131,132,133,134]. The negative contributions to compressibility obtained in these papers do not violate the stability of the quantum vacuum, since these contributions represent the corrections, which are small compared to the main value of the vacuum compressibility,

χ_{vac}^{- 1} \sim M_{Pl}^{4}

The excited vacuum (the de Sitter state) has the temperature

T = H / π

and the energy density

< ϵ_{vac} > \sim M_{Pl}^{2} H^{2}

. Then from Equation (74) it follows that the thermal fluctuations of the energy density in the Hubble volume are on the order of thermal energy energy density:

{〈{(Δ ϵ_{vac})}^{2}〉}_{V = V_{H}} \sim {〈ϵ_{vac}〉}^{2} .

(75)

This can be the reason of the two-fluid behaviour of the de Sitter state discussed in Section 6.4. The thermal fluctuations of dark energy play the role of dark matter in the same way as the oscillations of the dark energy in Ref.[125].

6.6. Cosmological Constant Problems

In principle, the phenomenological approaches to the dynamics of the vacuum energy density may produce different power-law decays. Examples are Equation (72) and Equation (). However, it is not excluded that these two asymptotic laws may correspond to different epochs.

So, if this speculative approach in Ref. Section 6.4 iworks, the equation (73) may solve all the cosmological constant problems:

1) why the cosmological constant is not large;

2) why the dark energy is on the order of dark matter;

3) why they have the present value.

7. From de Sitter to Black Hole Thermodynamics

7.1. De Sitter vs Black Hole

The thermodynamics of de Sitter state is very different from the thermodynamics of black holes. Black hole is the compact object. The temperature of the Hawking radiation

T_{H}

from the black hole horizon is well determined, which is also supported by the condensed matter analogs.[135] On the other hand, the origin of the black hole entropy is still not clear, although it can be determined from the equation

d M = T_{H} d S

, assuming that the laws of thermodynamics are applicable to this compact object.

On the contrary, the de Sitter state is not the compact object. It is the homogeneous vacuum state without boundaries, which has the homogeneous energy density as the local quantity. The local energy density allows us to introduce also the local temperature

T = H / π

. This local temperature can be measured by any detector which is stationary with respect to the shift velocity and which measures for example the rate of the ionization of an atom,

w \propto exp (- E / T)

7.2. Entropy of Expanding, Contracting and Static de Sitter

However, the de Sitter state allows us to probe the origin of the black hole entropy. For that we must consider three different states of the de Sitter quantum vacuum: expanding de Sitter with

H > 0

, contracting de Sitter with

H < 0

and the fully static vacuum. Let us start with the fully static de Sitter metric:

d s^{2} = - (1 - H^{2} r^{2}) d t^{2} + \frac{d r^{2}}{1 - H^{2} r^{2}} + r^{2} d Ω^{2} .

(76)

This metric has singularity at the cosmological horizon, which requires the proper attention. In one approach this static configuration can be considered as the intermediate symmetric state between the two states with broken time reversal symmetry – the expanding and contracting states. The same consideration of the static hole as the intermediate state between black and white holes see in Ref. [81].

The contracting de Sitter vacuum has negative Hubble parameter,

H < 0

. That is why its local temperature is negative,

T = H / π < 0

, and the local entropy is also negative,

s_{contracting} = 3 H / 4 G = - 3 / (4 G r_{H}) < 0

. The total entropy in the Hubble volume of contracting de Sitter is

S_{contracting} = s_{contracting} V_{H} = - \frac{A}{4 G},

(77)

where A is the area of the cosmological horizon. That is why the entropy of the static de Sitter as the intermediate state between the states with positive and negative entropies is zero. Correspondingly the temperature of this state must be infinite, which is consistent with the singularity at the horizon, see also Ref.[136].

7.3. Gravastar —Black Hole with de Sitter Core

The connection between the black hole and de Sitter appears, when we consider the black hole obtained by the transformation of the gravastar.[14] The gravastar is an object, which contains the de Sitter vacuum inside the black hole horizon.[137,138,139] We consider the gravastar in which the black hole horizon coincides with the de Sitter horizon,

r_{bh} = r_{H}

(the metric in the state with the critical value of the mass parameter

m = 2 M G | H | = 1

at which two horizons merge is illustrated in Fig. 1 of Ref. [140]). Such gravastar is stationary, that is why it has no Hawking radiation and its entropy is zero. In the Painlevé-Gullstrand form the metric of such gravastar is given by Equation (1) with the following shift velocity:

\begin{matrix} v (r) = - \sqrt{\frac{r_{H}}{r}}, r > r_{H}, \end{matrix}

(78)

\begin{matrix} v (r) = - \frac{r}{r_{H}}, r < r_{H} . \end{matrix}

(79)

Here

r_{H} = 1 / | H | = r_{bh}

, where

r_{bh} = 2 M G

and

M = 1 / (2 G | H |)

is the mass of the black hole, which is formed by the de Sitter core.

The shift velocity

v (r)

must be continuous across the horizon, i.e. there is no jump in the shift velocity, while the gradient of the shift velocity

d v / d r

experiences jump at the horizon. The shift velocity

v (r)

is negative both outside and inside the horizon. Since the shift velocity is negative in the de Sitter core, this means that the de Sitter spacetime in this gravastar is contracting,

v (r) = H r = - r / r_{H} < 0

, i.e. the Hubble parameter is negative,

H = - 1 / r_{H} < 0

7.4. Entropy of Black Hole from Negative Entropy of Contracting de Sitter

According to Equation (77) the region of the contracting de Sitter core of the gravastar has negative entropy,

S_{contracting} = - A / 4 G

. That is why the gravastar is unstable towards the shrinking of the de Sitter region, since this leads to the increase of the entropy of the whole system due to decrease of the negative entropy of the contracting de Sitter state. Due to the energy conservation the shrinking of the volume of the de Sitter core leads to formation of the singularity ar

r = 0

, where the mass becomes concentrated. In the final state – the black hole – the de Sitter region with negative entropy fully disappears by shrinking to the singularity with mass M. The resulting black hole with mass M acquires the positive entropy,

A / 4 G

S_{BH} = S_{gstar} - S_{contracting} = 0 - s_{contracting} V_{H} = \frac{A}{4 G} .

(80)

The black hole entropy is also concentrated in the singularity, together with the curvature

R

and mass M.[14] This again supports the holographic connection between the entropy of bulk, which is concentrated in the singularity, and the surface entropy of the black hole horizon.

Equation (80) allows to interpret the zero value of the entropy of the gravastar in terms of the cancellation of entropies of two horizons. In the initial gravastar state the entropy of the contracting de Sitter horizon fully compensates the entropy of the black hole horizon:

S_{gstar} = S_{contracting} + S_{BH} = - \frac{A}{4 G} + \frac{A}{4 G} = 0 .

(81)

7.5. White Hole and Anti-Gravastar

In the same way the anti-gravastar can be obtained as the white hole with the de Sitter core. This object has the following shift velocities:

\begin{matrix} v (r) = \sqrt{\frac{r_{H}}{r}}, r > r_{H}, \end{matrix}

(82)

\begin{matrix} v (r) = \frac{r}{r_{H}}, r < r_{H} . \end{matrix}

(83)

It is obtained from the pure white hole, which has the negative horizon entropy

S_{WH} = - A / 4 G

,81,82] by growing the de Sitter state in its core with positive entropy. In the anti-gravastar state the entropies of two horizons cancel each other in the same way as in the gravastar:

S_{antigstar} = S_{expanding} + S_{WH} = \frac{A}{4 G} - \frac{A}{4 G} = 0 .

(84)

It is important that the coordinate singularities in the metric of gravastar and in the metric of anti-gravastar can be smoothly removed by deformation. That is why these objects do not depend on the choice of the coordinate systems, and thus they are equivalent to the fully static black hole with the fully static de Sitter core:

\begin{matrix} d s^{2} = - (1 - 2 G M / r) d t^{2} + \frac{d r^{2}}{1 - 2 G M / r} + r^{2} d Ω^{2}, r > 2 M G = 1 / H, \end{matrix}

(85)

\begin{matrix} d s^{2} = - (1 - H^{2} r^{2}) d t^{2} + \frac{d r^{2}}{1 - H^{2} r^{2}} + r^{2} d Ω^{2}, r < 2 M G = 1 / H . \end{matrix}

(86)

This again supports the zero entropy of these gravastars.

7.6. Gibbs-Duhem and Black Hole Thermodynamics

Let us show, that the modified Gibbs-Duhem relation in Equation (46) is applicable also to the thermodynamics of black holes. As distinct from the de Sitter state, the black hole is the compact object, and its thermodynamics connects the global parameters, such as mass M, entropy of horizon, total electric charge Q and total angular momentum J. This global thermodynamics can be described by the integral form of the Gibbs-Duhem relation in Equation (46). The curvature here comes from the central singularity:[141]

R = 8 π M G δ (r) .

(87)

Since the energy density here is

ϵ = M δ (r)

, the integration of the right-hand-side of Equation (46) over space gives for the Schwarzschild black hole:

T_{BH} S_{BH} = M - \int d^{3} r \sqrt{- g} K R = \frac{M}{2} .

(88)

Here

T_{BH} = \frac{1}{8 π M G}

is the Hawking temperature and

S_{BH} = A / 4 G

is the Bekenstein-Hawking entropy. The Equation (88) is valid also for the white hole, where temperature and entropy are opposite to that of the black hole with the same mass,[81]

T_{WH} (M) = - T_{BH} (M)

and

S_{WH} (M) = - S_{BH} (M)

In principle, the central singularity in the black hole may spontaneously loose the spherical symmetry, forming for example a kind of rigid top. This in turn may influence the shape of the event horizon. This is similar to the deformations of the cosmological horizon by masses concentrated on vertices of Platonic solids deep within the Hubble volume.[142]

7.7. Entropy of the Schwarzschild-de Sitter Cosmological Horizon

Let us consider the possible application of the modified Gibbs-Duhem relation to the Schwarzschild-de Sitter (SdS) black hole. We discuss the simple case of the Nariai limit, when the black hole horizon approaches the cosmological horizon,

r_{b} \to r_{0} - 0

and

r_{c} \to r_{0} + 0

, where

r_{0} = {(G M / H^{2})}^{1 / 3} = \frac{1}{\sqrt{3} H} .

(89)

In this limit the temperatures of the horizons approach the Bousso-Hawking value:[143]

T_{b} = T_{c} = \frac{\sqrt{3}}{2 π} H = \frac{1}{6 π G M} .

(90)

The entropy of the cosmological horizon

S_{c}

can be obtained by integration of the right-hand-side of Equation (46) over space inside the cosmological horizon with radius

r_{0}

T_{c} S_{c} = M - \int_{r < r_{0}} d^{3} r \sqrt{- g} K R .

(91)

Since we discuss here the Nariai limit, one obtains:

T_{c} S_{c} = M - \int_{r < r_{0}} d^{3} r \sqrt{- g} K R = M - \frac{M}{2} + \frac{3 H^{2}}{4 π} \frac{4 π r_{0}^{3}}{3} = \frac{3}{2} M .

(92)

and the entropy of the cosmological horizon:

S_{c} = \frac{3 M}{2 T_{c}} = \frac{π r_{0}^{2}}{G} = \frac{A}{4 G} .

(93)

This again agrees with the Gibbons-Hawking entropy, although this holographic connection is valid only in the Narai limit.

7.8. Heat Exchange between Black Holes in the Multi-Metric Ensemble

The thermodynamic character of the black hole objects can be tested using the multi metric ensemble in Sec. Section 4. Let us consider ensemble of n sub-universes in the same coordinate spacetime,

S = - \int d^{4} x \sum_{n} L_{n}

, but with with different metrics

g_{μ ν (n)}

, different gravitational couplings

K_{n}

, and the corresponding individual black holes with masses

M_{n}

. If one introduces the energy exchange between these sub-universes, then the masses

M_{n}

will be varied at the fixed total mass

M = \sum_{n} M_{n}

of the whole Universe. In the thermal equilibrium, which corresponds to the maximum of the total entropy, the individual metrics approach the common metric, and the whole system corresponds to the Universe with the gravitational coupling

K = \sum_{n} K_{n}

and with the black hole of mass M. The equilibrium masses

M_{n}

of the individual substates approach the values:

M_{n} = M \frac{K_{n}}{K} .

(94)

In this equilibrium states, the Hawking temperature of the black hole with mass M in the whole ensemble coincides with Hawking temperatures of the individual black holes in each gravitational sub-states:

\frac{1}{T_{n}} = \frac{d S_{n}}{d M_{n}} = \frac{d S}{d M} = \frac{1}{T_{H}} .

(95)

This is the effect of thermalization.

8. Black and White Holes Entropy from Macroscopic Quantum Tunneling

8.1. Collective Canonically Conjugate Variables for Schwarzschild Black Hole

Considering the thermodynamics of gravity systems we used the thermodynamically conjugate variables – the gravitational coupling

K = 1 / 16 π G

and the scalar curvature

R

, which as the covariant quantity may serve as one of the thermodynamical characteristics of the macroscopic matter.[87] These variables are the local thermodynamic variables, which are similar to temperature, pressure, chemical potential, number density, etc., in condensed matter physics.

The gravitational coupling K is determined by the microscopic physics, but in the description of gravity as macroscopic phenomenon it is the collective variable. In the superfluid ³He-A with Weyl fermionic quasiparticles, both the coupling K in the effective gravity and the fine structure “constant“

α

in the effective electrodynamics are determined by physics on the microscopic (atomic) level.[25] In these effective theories, one obtains

K \propto Δ_{0}^{2}

and

1 / α \propto ln (Δ_{0} / T)

, where

Δ_{0}

is the gap amplitude and T is the temperature of the liquid. Here

Δ_{0}

and T play correspondingly the role of the ultraviolet cut-off

M_{Pl}

and of the infrared cut-off. For the relativistic quantum fields with massless particles, the infrared cut-off is either the temperature T or the strength of the fields. In the inhomogeneous superfluid (inhomogeneous vacuum) both K and

α

depend on coordinates. It is not surprizing that in the relativistic quantum vacuum there is also the connection between the gravitational coupling K and the coupling

α

in quantum electrodynamics as suggested in Refs. [144,145,146,147,148,149,150]

Now, for the discussion of the quantum-mechanical tunneling of the macroscopic objects we need the collective dynamical variables, instead of the thermodynamic variables. The canonically conjugate dynamical variables, which are relevant for the black hole, are the gravitational coupling K and the horizon area

A = 4 π R^{2}

. Bekenstein [151] proposed that A is an adiabatic invariant and thus can be quantized according to the Ehrenfest principle, that classical adiabatic invariants may correspond to observables with discrete spectrum. So the area of the horizon A is the proper candidate for the quantum mechanics of the black hole.

8.2. Modified First Law of Black Hole Thermodynamics

Let us first consider how these variables enter the black hole thermodynamics. For that it is convenient to use the redefined gravitational coupling

\tilde{K} = 4 π K = 1 / 4 G

. In terms of this coupling the Hawking temperature of Schwarzschild black hole and its Bekenstein entropy are:

T_{BH} = \frac{\tilde{K}}{2 π M}, S_{BH} = \frac{π M^{2}}{\tilde{K}} = A \tilde{K} .

(96)

\tilde{K}

is a global thermodynamic variable, one obtains the following modification of the first law of black hole thermodynamics:

\begin{matrix} d S_{BH} = d (A \tilde{K}) = π d (M^{2} / \tilde{K}) = = - π \frac{M^{2}}{{\tilde{K}}^{2}} d \tilde{K} + 2 π \frac{M}{\tilde{K}} d M \end{matrix}

(97)

\begin{matrix} d S_{BH} = - A d \tilde{K} + \frac{d M}{T_{BH}} . \end{matrix}

(98)

This modification is similar to the modification in terms of the moduli fields.[152] But in our case the thermodynamic variable, which is conjugate to the thermodynamic variable

\tilde{K}

, is the product of the black hole area and the black hole temperature,

A T_{BH}

. On the other hand in dynamics,

\tilde{K}

and A are canonically conjugate variables, see Sec.Section 8.4.

In general, the variable

\tilde{K}

is local and depends on space coordinate, but in the same way as for the moduli fields,[152] the black hole thermodynamics is determined by the asymptotic value of K at spatial infinity. In Equation (98),

\tilde{K} \equiv \tilde{K} (\infty)

is the global quantity, which characterizes the quantum vacuum in full equilibrium, i.e. far from the black hole.

Also, the variable

\tilde{K}

allows us to study the transition to the vacuum without gravity, i.e. to the vacuum where

\tilde{K} \to \infty

and thus

G \to 0

, see Sec.Section 8.4.

8.3. Adiabatic Change of Coupling K and Adiabatic Invariant

Let us change the coupling

\tilde{K}

and the black hole mass M adiabatically, i.e. at constant entropy of the black hole. Then the equation

d S_{BH} = 0

gives

\frac{d M}{d \tilde{K}} = A T_{BH} = \frac{M}{2 \tilde{K}} .

(99)

This shows that

M^{2} / \tilde{K} = const

is the adiabatic invariant for the spherical electrically neutral black hole. Thus according to the Bekenstein conjecture [151], it can be quantized in quantum mechanics:

\frac{M^{2}}{\tilde{K}} = a N .

(100)

Here N is integer, and a is some fundamental dimensionless parameter of order unity. If this conjecture is correct, one obtains the quantization of the entropy of Schwartzschild black hole:

S_{BH} (N) = π \frac{M^{2}}{\tilde{K}} = π a N .

(101)

The Bekenstein idea on the role of adiabatic invariants in quantization of the black hole requires further consideration, see some approaches to that in Refs. [153,154,155,156,157,158]. In particular, the similarity between the energy levels of Schwarzschild black hole and the hydrogen atom has been suggested. [159,160] We leave this problem for the future. This consideration should be supported by microscopic theory, see e.g. [161].

In this respect, the condensed matter analogs can be useful, since in the condensed matter systems the physics is known both on macro and micro (atomic) levels. One example is provided by consideration of the quantum nucleation of the vortex ring in moving superfluids – the vortex instanton. It shows that the corresponding entropy which determines the nucleation process,

exp (- S_{ring})

, is quantized:

S_{ring} (N) = 2 π N .

(102)

Here N is the number of atoms involved in the process of the vortex instanton, see Sec. 26.4 and Eqs.(26.20)-(26.21) in Ref. [25]. This would correspond to the parameter

a = 2

in Equation (100).

8.4. A and K as Canonically Conjugate Variables and Black-Hole—White-Hole Quantum Tunneling

The canonically conjugate variables A and K allow us to consider the quantum mechanical tunneling from the black hole to the white hole – the process discussed in Refs. [162,163,164,165,166,167,168,169,170,171] and in references therein. In the semiclassical description of this macroscopic quantum tunneling, the trajectory in the

(\tilde{K}, A)

phase space must be considered, which in the complex plane connects the black and white holes.

Note the difference from consideration in Section 8.3, where

\tilde{K}

varies in the adiabatic regime, i.e. at fixed entropy

S_{BH}

, while the area A, temperature

T_{BH}

and mass M follow the variation of

\tilde{K}

. In the dynamic regime, which is relevant for the description of quantum tunnelling, the parameter

\tilde{K}

varies at fixed energy (fixed mass M of the black hole), while the area A, the temperature

T_{BH}

and entropy

S_{BH}

follow the variation of

\tilde{K}

As in the case of the semiclassical consideration of the Hawking radiation in terms of the quantum tunneling, we shall use the Painleve-Gullstrand coordinate system with the metric:

d s^{2} = - d t^{2} (1 - v^{2}) - 2 d t d r \cdot v + d r^{2},

(103)

where for the Schwartzschild black hole one has

v (r) = \mp \hat{r} \sqrt{\frac{R}{r}} = \mp \hat{r} \sqrt{\frac{M}{2 r \tilde{K}}} = \mp \hat{r} \sqrt{\frac{2 M G}{r}},

(104)

where R is the radius of the horizon; the minus sign corresponds to the black hole and the plus sign describes the white hole. In the theory with the variable gravitational coupling, the sign changes at the singularity

\tilde{K} = \infty

(i.e. at

G = 0

), when the black hole shrinks to a point and then expands as a white hole. The point

\tilde{K} = \infty

, where gravity disappears, serves as the branch point, where the velocity of the freely falling observer changes sign.

The vector

v

is normal to the surface of the horizon, and when it changes sign, this means that the horizon area A changes sign: it crosses zero at

\tilde{K} = \infty

and becomes negative on the white-hole side of the process,

A \to - A

. This also could mean that due to connection between the area and entropy the white hole may have negative entropy. This is what we shall discuss in the Section 8.5.

The quantum tunneling exponent is usually determined by the imaginary part of the action on the trajectory, which transforms the black hole to white hole. In terms of Euclidean action one has:

p_{BH \to WH} \propto exp (- I_{BH \to WH}), I_{BH \to WH} = \int_{C} A ({\tilde{K}}^{'}) d {\tilde{K}}^{'} .

(105)

Here the semiclassical trajectory C is at

M = const

, and thus

A ({\tilde{K}}^{'}) = \pm π M^{2} / {({\tilde{K}}^{'})}^{2}

. Along this trajectory the variable

K^{'}

changes from

\tilde{K}

to the branch point at

{\tilde{K}}^{'} = \infty

, and then from

{\tilde{K}}^{'} = \infty

{\tilde{K}}^{'} = K

along the other branch, where the area

A ({\tilde{K}}^{'}) < 0

. The integral gives the tunneling exponent of the transition to the white hole

I_{BH \to WH} = 2 π M^{2} \int_{\tilde{K}}^{\infty} \frac{d {\tilde{K}}^{'}}{{\tilde{K}}^{' 2}} = 2 π \frac{M^{2}}{\tilde{K}} .

(106)

The tunneling exponent in Equation (106) can be expressed in terms of the black hole entropy in Eq (96), and for the probability of transition one obtains:

p_{BH \to WH} \propto exp (- 2 π M^{2} / \tilde{K}) = exp (- 2 S_{BH}) .

(107)

It is important that Equation (107) contains exactly twice the black hole entropy. This allows us to consider again the entropy of the white hole.

8.5. Negative Entropy of White Hole

The connection between the probability of the transition and the thermodynamic fluctuations[172] is applicable also to the transition between the black and white holes. The total change of the entropy in this process is

Δ S = S_{WH} - S_{BH}

. According to Equation (109) this change is equal to

- 2 S_{BH}

. Then, from equation

S_{WH} - S_{BH} = - 2 S_{BH}

, one obtains that the entropy of the white hole is equal with the opposite sign to the entropy of the black hole with the same mass:

S_{WH} (M) = - S_{BH} (M) .

(108)

This means that the white hole, which is obtained by the quantum tunneling from the black hole and thus has the same mass M as the black hole, has the negative temperature

T_{WH} = - T_{BH}

and the negative area

A_{WH} = - A_{BH}

, which together produce the negative entropy

S_{WH} = - S_{BH}

Such anti-symmetry between the black and white holes is similar to the anti-symmetry between the expanding and contracting de Sitter state discussed in Section 7.2.

The discussed transition from the black hole to the white hole with the same mass M is not the thermodynamic transition. It is the quantum process of tunneling between the two quantum states. It is one of many routes of the black hole evaporation, including formation of small white hole on the late stage of the decay. [162,163,164,165,166,167,168,169,170,171] The uniqueness of this particular route, the hidden information and the (anti)symmetry between the black and white holes are combined to produce the negative entropy of the white hole.

8.6. Black Hole to White Hole Transition as Series of the Hawking Radiation Co-Tunneling

Let us show that the result (107) with twice the black hole entropy is supported by consideration of the conventional Hawking radiation of particles from the black hole. The tunneling exponent of radiation can be expressed in terms of the change in the entropy of the black hole after radiation,

p \propto e^{Δ S_{BH}}

, see Refs. [173,174,175,176]. This demonstrates that the Hawking radiation process has the thermodynamic meaning as thermodynamic fluctuation.[172]

We consider the process of the co-tunneling, in which the particle escapes the black hole by quantum tunneling, and then this particle tunnels to the white hole through the white hole horizon (this is the analog of the electron tunneling via an intermediate virtual state in electronic systems [177,178]). This process takes place at the fixed total mass M. The tunneling exponent for this process to occur is

e^{(Δ S_{BH} + Δ S_{WH})}

. Summation of all the processes of the tunneling of matter from the black hole to the formed white hole gives finally Equation (107):

p \propto e^{\sum (Δ S_{BH} + Δ S_{WH})} = e^{2 \sum Δ S_{BH}} = exp (- 2 S_{BH}) .

(109)

Here we took into account the (anti)symmetry in the dynamics of black and white holes in the process of quantum tunneling,

\sum Δ S_{BH} = \sum Δ S_{WH}

8.7. Emission of Small Black Holes vs Hawking Radiation

The principle that the macroscopic quantum tunneling can be considered as thermodynamic fluctuation can be also applied to the process of the creation of pairs black holes,[179] to the process of splitting of the black hole into two or several smaller black holes with the same total mass, see e.g. Ref.[180], and to other processes with macroscopic objects. For example, the probability of the decay of the black hole with mass M into two black holes with

M_{1} + M_{2} = M

is:

\begin{matrix} p (M \to M_{1} + M_{2}) \propto \end{matrix}

(110)

\begin{matrix} e^{S_{BH} (M_{1}) + S_{BH} (M_{2}) - S_{BH} (M_{1} + M_{2})} = e^{- 8 π G M_{1} M_{2}} . \end{matrix}

(111)

In the particular limit case

m = M_{1} ≪ M_{2} \approx M

, this channel of the black hole decay describes the emission of the small black hole with mass m by the large black hole with mass M:

p (m, M) \propto exp (- \frac{m}{T_{BH} (M)}), m ≪ M .

(112)

This shows that the macroscopic tunneling process of emission of a small black hole by a large black hole is governed by the same Hawking temperature

T_{BH} (M) = 1 / (8 π G M)

as the Hawking radiation of a particle, which tunnels across the horizon.

However, there is the difference. In Equation (112) the quadratic term

m^{2}

is neglected. In general case, one obtains from Equation (110):

p (m, M - m) \propto exp (- 8 π G m (M - m)) .

(113)

This equation demonstrates the effect of back reaction – the correction to the Hawking radiation caused by the reduction of the black hole mass after the radiation of a small black hole. The similar correction due to the back reaction in the process of radiation of particles was obtained by Parikh and Wilczek [176] (see also Ref.[173]):

p (ω, M - ω) \propto exp (- 8 π G ω (M - \frac{ω}{2})),

(114)

where

ω

is the energy of the emitted particle. As distinct from Equation (113) for emission of a small black hole, the Equation (114) contains the factor

1 / 2

. The reason for such difference is that in case of the emission of a small black hole, the probability of emission contains the extra term compared to the emission of particles – the entropy of the emitted black hole,

S (m) = 4 π G m^{2}

p (m, M - m) \propto exp (- 8 π G m (M - \frac{m}{2}) + 4 π G m^{2}) .

(115)

As a result the Equation (113) is restored. This also coincides with the result for the radiation of the self-gravitating shell.[181]

Equation (110) can be extended to emission of several black holes. For example, the probability of emission of N black holes with masses

m = M / N

is:

\begin{matrix} p (M \to m N) \propto exp (- 4 π G M^{2} (1 - \frac{1}{N})) . \end{matrix}

(116)

For large N this corresponds to the probability of the destruction of the black hole by explosion within the particular channel:

\begin{matrix} p_{N \to \infty} \propto exp (- S_{BH}) . \end{matrix}

(117)

There are many channels of the destruction of the black hole in quantum tunnelling. The black hole entropy

S_{BH}

can be estimated using the probability of the black hole explosion in a single quantum event. Equation (117) suggests that the entropy of the black hole can be determined by the number of channels of its destruction.

9. Conclusion

The starting point of our consideration was that matter immersed in the de Sitter vacuum feels this vacuum as the heat bath with the local temperature

T = H / π

T_{GH} = H / 2 π

. The reason for such relation is the specific symmetry of the de Sitter space-time, which is similar to the invariance under translations in the Minkowski vacuum.

There are also the discrete symmetries, which are important for consideration of the thermodynamics of the de Sitter. It represents one of the two degenerate states formed by the broken time reversal symmetry. These states are the expanding and contracting de Sitter states. They are obtained from each other by the time reversal transformation,

t \to - t

. Another broken discrete symmetry corresponds to the reversal of the sign of the scalar curvature,

R \to - R

. This symmetry operation transforms the de Sitter state to the anti-de Sitter. This symmetry is spontaneously broken by the linear in

R

term in the Einstein action,

\sqrt{- g} K R

The local thermodynamics of the de Sitter state in the Einstein gravity gives rise to the Gibbons-Hawking area law for the total entropy inside the cosmological horizon. We extended the consideration of the local thermodynamics to the

f (R)

gravity and obtained the same area law, but with the modified gravitational coupling

K = d f / d R

. The agreement with the traditional global thermodynamics of de Sitter supports the suggestion that the de Sitter vacuum is the thermal state with the local temperature

T = H / π

, and that the local thermodynamics is based on the thermodynamically conjugate gravitational variables K and

R

. This pair of the non-extensive gravitational variables is similar to the pair of the electrodynamic variables, electric field

E

and electric induction

D

, which participate in the thermodynamics of dielectrics. The gravitational variables modify the thermodynamic Gibbs-Duhem relation, due to which the thermal properties of the de Sitter state become similar to that of the Zel’dovich stiff matter and of the non-relativistic Fermi liquid.

The local temperature

T = H / π

leads to the multiple creation of particles, if even only single electron is introduced to the de Sitter vacuum. This results in the thermal instability of the de Sitter state towards the formation of matter, and to further thermalization of this matter by the de Sitter heat bath. The process of thermalization of matter by the de Sitter heat bath, which takes place without the effects from the cosmological horizon, leads to the decay of the vacuum energy density. As distinct from this process, the possibility of instability of the de Sitter state due to the Hawking radiation from the cosmological horizon is still controversial.

We considered two scenarios of the vacuum decay, which give two different power laws of decay. One of them reproduces the result of the Padmanabhan model.[113] The second one is based on the thermal fluctuations in the de Sitter heat bath. It leads to the reasonable values of the dark energy and dark matter in the present time, and these values are not sensitive to the initial state of the Universe. This scenario suggests the simultaneous solution of three cosmological constant problems: why the cosmological constant is not large; why the dark energy is on the order of dark matter; and why they have the present order of magnitude.

Using local thermodynamics with the local temperature

T = H / π

, we obtained the connection between the bulk entropy of the Hubble volume, and the surface entropy of the cosmological horizon

S_{hor} = A / 4 G

. This suggests a kind of the bulk-surface correspondence, which may have the holographic origin.[182,183,184] It would be interesting to check this correspondence using the more general extensions of the Einstein gravity and also different types of the generalized entropy.[86,185,186,187,188] It is important that such connection takes place only in the

3 + 1

spacetime, where there is the special symmetry due to which both gravitational variables K and

R

have the mass dimension 2, the same as the electrodynamic variables, electric field

E

and electric induction

D

We also discussed the thermodynamics of de Sitter in the frame of the statistical ensemble of the multi-metric gravities. The heat exchange between different "sub-Universes" in the ensemble leads to the common de Sitter expansion with the common temperature

T = H / π

. Application of the local thermodynamics to the entropy of the Schwarzschild black hole was also considered. We obtained the Bekenstein-Hawking entropy of black hole from the negative entropy of the contracting de Sitter core of the gravastar object.

9.1. Thermodynamic Variables vs Canonical Variables

We considered the dynamics and thermodynamics of the black hole in case of the varying gravitational coupling

\tilde{K}

. The gravitational coupling

\tilde{K}

serves as the thermodynamic variable, which is thermodynamic conjugate to

A_{BH} T_{BH}

, where

A_{BH}

and

T_{BH}

are correspondingly the area of the black hole horizon and Hawking temperature. The corresponding first law of the black hole is modified, see Equation (98). The corresponding adiabatic invariant is the entropy

S_{BH} = \tilde{K} A_{BH}

, and it is this invariant which should be quantized, if the Bekenstein conjecture is correct. This is in agreement with observation of Ted Jacobson [189], that it is the entropy that does not change under renormalization of

\tilde{K}

, rather than the area. This suggests the alternative quantization scheme for the black hole. While

\tilde{K}

and

A_{BH}

are dimensionful and cannot be quantized, the entropy is dimensionless and thus can be quantized in terms of some fundamental numbers.

On the quantum level the dynamically conjugate variables of the black hole physics are

\tilde{K}

and

A_{BH}

. This allows us to consider the transition from the black hole to the white hole as quantum tunneling in the semiclassical approximation, which is valid when the action is large. The classical trajectory of the black hole crosses the branch point at

\tilde{K} = \infty

, and then continues along the other branch, where the area

A (\tilde{K}) < 0

, which corresponds to the white hole. The obtained tunneling exponent

exp (- 2 S_{BH})

demonstrates that the transition can be considered as thermodynamic fluctuation, if the entropy of the white hole (with the same mass M as the black hole) is negative,

S_{WH} = - S_{BH}

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Thermodynamics and Decay of de Sitter Vacuum

Abstract

1. Introduction

2. De Sitter State as Heat Bath for Matter

2.1. Atom in de Sitter Environment as Thermometer

2.2. Decay of Composite Particles in de Sitter Spacetime

2.3. Triplication of Particles in de Sitter Spacetime

2.4. Connection between the Local and Hawking Temperatures

2.5. Two Detectors: Exited Atom vs Ionized Atom

2.6. Radiation of Photons by Atom in de Sitter Environment

2.7. Accelerating Detector: Is There Connection between the Local Process and Unruh Radiation?

3. Thermodynamics of the de Sitter State

3.1. De Sitter Symmetry and de Sitter Heat Bath

3.2. From Local Temperature to Local Entropy

3.3. De Sitter Vacuum, Fermi Liquid and Cosmological Constant Problem

3.4. Hubble Volume Entropy vs Entropy of the Cosmological Horizon

4. Thermodynamics from the Heat Transfer in the Multi-Metric Gravity Ensemble

4.1. Multi-Metric Gravity

4.2. Heat Exchange in Multi-Metric Gravity

4.3. Thermodynamics from the Multi-Metric Ensemble

4.4. Regularization vs Thermalization

4.5. Coherence vs Thermalization

4.6. De Sitter Contribution to Chiral Anomaly

5. Thermodynamics of de Sitter State and f ( R ) Gravity

5.1. Thermodynamic variables in f ( R ) gravity

5.2. Gibbs-Duhem Relation in f ( R ) Gravity

5.3. Entropy of Cosmological Horizon in Terms of Effective Gravitational Coupling

5.4. Example of Quadratic Gravity

6. From de Sitter Thermodynamics to de Sitter Decay

6.1. De Sitter State as Thermal Bath for Matter

6.2. De Sitter Decay due to Thermalization of Matter by de Sitter Heat Bath

6.3. Connection to Holographic Principle

6.4. De Sitter Decay and Zel’dovich Stiff Matter

6.5. Thermal Fluctuations in de Sitter State

6.6. Cosmological Constant Problems

7. From de Sitter to Black Hole Thermodynamics

7.1. De Sitter vs Black Hole

7.2. Entropy of Expanding, Contracting and Static de Sitter

7.3. Gravastar —Black Hole with de Sitter Core

7.4. Entropy of Black Hole from Negative Entropy of Contracting de Sitter

7.5. White Hole and Anti-Gravastar

7.6. Gibbs-Duhem and Black Hole Thermodynamics

7.7. Entropy of the Schwarzschild-de Sitter Cosmological Horizon

7.8. Heat Exchange between Black Holes in the Multi-Metric Ensemble

8. Black and White Holes Entropy from Macroscopic Quantum Tunneling

8.1. Collective Canonically Conjugate Variables for Schwarzschild Black Hole

8.2. Modified First Law of Black Hole Thermodynamics

8.3. Adiabatic Change of Coupling K and Adiabatic Invariant

8.4. A and K as Canonically Conjugate Variables and Black-Hole—White-Hole Quantum Tunneling

8.5. Negative Entropy of White Hole

8.6. Black Hole to White Hole Transition as Series of the Hawking Radiation Co-Tunneling

8.7. Emission of Small Black Holes vs Hawking Radiation

9. Conclusion

9.1. Thermodynamic Variables vs Canonical Variables

References

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5. Thermodynamics of de Sitter State and $f (R)$ Gravity

5.1. Thermodynamic variables in $f (R)$ gravity

5.2. Gibbs-Duhem Relation in $f (R)$ Gravity