# The Critical Phenomena and Thermodynamics of the Reissner-Nordstrom-de Sitter Black Hole

Authors: Ren Zhao; Mengsen Ma; Huihua Zhao; Lichun Zhang
Journal: Advances in High Energy Physics
 (2014)

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## Abstract

It is wellknown that there are two horizons for the Reissner-Nordstrom-de Sitter spacetime, namely, the black hole horizon and the cosmological one. Both horizons can usually seem to be two independent thermodynamic systems; however, the thermodynamic quantities on both horizons satisfy the laws of black hole thermodynamics and are not independent. In this paper by considering the relations between the two horizons we give the effective thermodynamic quantities in Reissner-Nordstrom-de Sitter spacetime. The thermodynamic properties of these effective quantities are analyzed; moreover, the critical temperature, critical pressure, and critical volume are obtained. We also discussed the thermodynamic stability of Reissner-Nordstrom-de Sitter spacetime.


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## Body

## 1. Introduction

Black hole physics, especially the black hole thermodynamics, refer directly to the theories of gravity, statistical physics, particle physics, field theory, and so forth. This makes the field concerned by many physicists [1–6]. Although the complete statistical description of black hole thermodynamics is still unclear, the research on the properties of black hole thermodynamics is prevalent, such as Hawking-Page phase transition [7], and critical phenomena. More interestingly, the research on the charged and nonrotating RN-AdS black hole shows that there exists a similar phase transition to the van der Waals-Maxwell vapor-liquid phase transition [8, 9].Motivated by the AdS/CFT correspondence [10], where the transitions have been related with the holographic superconductivity [11, 12], the subject of the phase transitions of black holes in asymptotically anti-de Sitter (AdS) spacetime has received considerable attention [13–17]. The underlying microscopic statistical interaction of the black holes is also expected to be understood via the study of the gauge theory living on the boundary in the gauge/gravity duality.Recently, by considering the cosmological constant correspond to pressure in general thermodynamic system, namely,(1)
P
=
-
1
8
π
Λ
=
3
8
π
1
l
2
,
the thermodynamic volumes in AdS and dS spacetime are obtained [18–24]. The studies on phase transition of black holes have aroused great interest [25–31]. Connecting the thermodynamic quantities of AdS black holes to (
P
~
V
) in the ordinary thermodynamic system, the critical behaviors of black holes can be analyzed and the phase diagram like van der Waals vapor-liquid system can be obtained. This helps to further understand the black hole entropy, temperature, heat capacities, and so forth. It also has a very important significance in completing the geometric theory of black hole thermodynamics.As is well known, there are black hole horizon and cosmological horizon in the appropriate range of parameters for de Sitter spacetime. Both horizons have thermal radiation, but with different temperatures. The thermodynamic quantities on both horizons satisfy the first law of thermodynamics, and the corresponding entropy fulfills the area formula [23, 32, 33]. In recent years, the research on the thermodynamic properties of de Sitter spacetime has drawn a lot of attention [23, 32–36]. In the inflation epoch of early universe, the universe is a quasi-de Sitter spacetime. The cosmological constant introduced in de Sitter space may come from the vacuum energy, which is also a kind of energy. If the cosmological constant is the dark energy, the universe will evolve to a new de Sitter phase. To depict the whole history of evolution of the universe, we should have some knowledge on the classical and quantum properties of de Sitter space [23, 33, 37, 38].Firstly, we expect the thermodynamic entropy to satisfy the Nernst theorem [34, 35, 39]. At present a satisfactory explanation to the problem in which the thermodynamic entropy of the horizon of the extreme de Sitter spacetime does not fulfill the Nernst theorem is still lacking. Secondly, when considering the correlation between the black hole horizon and the cosmological horizon whether the thermodynamic quantities in de Sitter spacetime still have the phase transition and critical behavior like in AdS black holes. Thus it is worthy of our deep investigation and reflection to establish a consistent thermodynamics in de Sitter spacetime.Because the thermodynamic quantities on the black hole horizon and the cosmological one in de Sitter spacetime are the functions of massM, electric charge Q, and cosmological constant Λ. The quantities are not independent of each other. Considering the relation between the thermodynamic quantities on the two horizons is very important for studying the thermodynamic properties of de Sitter spacetime. Based on the relation we give the effective temperature and pressure of Reissner-Nordstrom-de Sitter(R-NdS) spacetime and analyze the critical behavior of the equivalent thermodynamic quantities. It is shown that when considering the relation between the two horizons in RN-dS spacetime there is the similar phase transition like the ones in van der Waals liquid-gas system and charged AdS black holes.The paper is arranged as follows. In Section2 we introduce the Reissner-Nordstrom-de Sitter(R-NdS) spacetime and give the two horizons and corresponding thermodynamic quantities. In Section 3 by considering the relations between the two horizons we obtain the effective temperature and the equivalent pressure. In Section 4 the critical phenomena of effective thermodynamic quantities are discussed. Finally we discuss and summarize our results in Section 5 (we use the units G
n
+
1
=
ℏ
=
k
B
=
c
=
1).


## 2. RN-dS Spacetime

The line element of the R-N SdS black holes is given by [32]
(2)
d
s
2
=
-
f
(
r
)
d
t
2
+
f
-
1
d
r
2
+
r
2
d
Ω
2
,
where
(3)
f
(
r
)
=
1
-
2
M
r
+
Q
2
r
2
-
Λ
3
r
2
.
The above geometry possesses three horizons: the black hole Cauchy horizon located at r
=
r
-, the black hole event horizon (BEH) located at r
=
r
+, and the cosmological event horizon (CEH) located at r
=
r
c, where r
c
>
r
+
>
r
-, the only real, positive zeroes of f
(
r
)
=
0.The equationsf
(
r
+
)
=
0 and f
(
r
c
)
=
0 are rearranged to
(4)
Q
2
=
r
+
r
c
(
1
-
r
c
2
+
r
c
r
+
+
r
+
2
3
Λ
)
,
2
M
=
(
r
c
+
r
+
)
(
1
-
r
c
2
+
r
+
2
3
Λ
)
.
The surface gravity on the black hole horizon and the cosmological horizon is, respectively,
(5)
κ
+
=
1
2
d
f
(
r
)
d
r
|
r
=
r
+
=
r
+
2
-
Q
2
-
r
+
4
Λ
2
r
+
3
=
(
r
+
-
r
c
)
2
r
+
2
(
1
-
(
r
c
2
+
2
r
+
r
c
+
3
r
+
2
)
(
r
c
r
+
-
Q
2
)
r
c
r
+
(
r
c
2
+
r
+
r
c
+
r
+
2
)
)
,
κ
c
=
1
2
d
f
(
r
)
d
r
|
r
=
r
c
=
r
c
2
-
Q
2
-
r
c
4
Λ
2
r
c
3
=
(
r
c
-
r
+
)
2
r
c
2
(
1
-
(
r
+
2
+
2
r
+
r
c
+
3
r
c
2
)
(
r
c
r
+
-
Q
2
)
r
c
r
+
(
r
c
2
+
r
+
r
c
+
r
+
2
)
)
.
The thermodynamic quantities on the two horizons satisfy the first law of thermodynamics [23, 33, 40, 41]:
(6)
δ
M
=
κ
+
2
π
δ
S
+
+
Φ
+
δ
Q
+
V
+
δ
P
,
δ
M
=
κ
c
2
π
δ
S
c
+
Φ
c
δ
Q
+
V
c
δ
P
,
where S
+
=
π
r
+
2, S
c
=
π
r
c
2, Φ
+
=
Q
/
r
+, Φ
c
=
-
(
Q
/
r
c
), V
+
=
(
4
π
/
3
)
r
+
3, V
c
=
(
4
π
/
3
)
r
c
3, P
=
-
(
Λ
/
8
π
).


## 3. Thermodynamic Quantity of RN-dS Spacetime

In Section2, we have obtained thermodynamic quantities without considering the relationship between the black hole horizon and the cosmological horizon. Because there are three variables M, Q, and Λ in the spacetime, the thermodynamic quantities corresponding to the black hole horizon and the cosmological horizon are functional with respect to M, Q, and Λ. The thermodynamic quantities corresponding to the black hole horizon are related to the ones corresponding to the cosmological horizon. When the thermodynamic property of charged de Sitter spacetime is studied, we must consider the relationship with the two horizons. Recently, by studying Hawking radiation of de Sitter spacetime, [42, 43] obtained that the outgoing rate of the charged de Sitter spacetime which radiates particles with energy ω is
(7)
Γ
=
e
Δ
S
+
+
Δ
S
c
,
where Δ
S
+ and Δ
S
c are Bekenstein-Hawking entropy difference corresponding to the black hole horizon and the cosmological horizon after the charged de Sitter spacetime radiates particles with energy ω. Therefore, the thermodynamic entropy of the charged de Sitter spacetime is the sum of the black hole horizon entropy and the cosmological horizon entropy:
(8)
S
=
S
+
+
S
c
.
Substituting (6) into (8), one can obtain
(9)
d
S
=
2
π
(
1
κ
+
+
1
κ
c
)
d
M
-
2
π
(
φ
+
κ
+
+
φ
c
κ
c
)
d
Q
+
π
3
(
r
+
3
κ
+
+
r
c
3
κ
c
)
d
Λ
.
For simplicity, we consider the case with constant. In this case the equation above turns into
(10)
d
S
=
2
π
(
1
κ
+
+
1
κ
c
)
d
M
+
π
3
(
r
+
3
κ
+
+
r
c
3
κ
c
)
d
Λ
.
From (4) and (5), we derive
(11)
d
r
c
=
d
M
r
c
κ
c
+
(
r
c
3
/
3
)
2
r
c
κ
c
d
Λ
,
d
r
+
=
d
M
r
+
κ
+
+
(
r
+
3
/
3
)
2
r
+
κ
+
d
Λ
.
Recently, the thermodynamic volume of RN-dS spacetime [23, 34] is given as
(12)
V
=
4
π
3
(
r
c
3
-
r
+
3
)
.
Substituting (11) into (12), one gets
(13)
d
V
=
4
π
(
r
c
κ
c
-
r
+
κ
+
)
d
M
+
2
π
3
(
r
c
4
κ
c
-
r
+
4
κ
+
)
d
Λ
.
Substituting (13) into (10), one can derive the thermodynamic equation of thermodynamic quantities in de Sitter spacetime [34]:
(14)
d
M
=
T
eff
d
S
-
P
eff
d
V
,
where the effective temperature is
(15)
T
eff
=
(
x
4
+
x
3
-
2
x
2
+
x
+
1
)
4
π
r
c
x
(
x
+
1
)
(
x
2
+
x
+
1
)
-
Q
2
4
π
r
c
3
x
3
(
x
+
1
)
(
x
2
+
x
+
1
)
×
(
1
+
x
+
x
2
-
2
x
3
+
x
4
+
x
5
+
x
6
)
.
The effective pressure is
(16)
P
eff
=
(
1
-
x
)
(
1
+
3
x
+
3
x
2
+
3
x
3
+
x
4
)
8
π
r
c
2
x
(
1
+
x
)
(
1
+
x
+
x
2
)
2
-
Q
2
(
1
-
x
)
(
1
+
2
x
+
3
x
2
-
3
x
5
-
2
x
6
-
x
7
)
8
π
r
c
4
x
3
(
1
+
x
)
(
1
-
x
3
)
(
1
+
x
+
x
2
)
,
where x
:
=
r
+
/
r
c and 0
<
x
<
1.From (15) and (16), when Q
=
0, the effective temperature and pressure are both greater than zero. This fulfills the stable condition of thermodynamic equilibrium. If considering the black hole horizon and the cosmological one as independent of each other, because of the different radiant temperatures on the two horizons, the spacetime is instable.Another problem of considering the black hole horizon and the cosmological one as independent of each other is that when the two horizons coincide, namely,(17)
r
+
/
c
2
=
1
±
1
-
4
Q
2
Λ
2
Λ
=
r
0
2
,
from (4), the surface gravity κ
+
/
c
=
0; thus the temperature on the black hole horizon and the temperature on the cosmological horizon are both zero. However, both horizons have nonzero area, which means that the entropy for the two horizons should not be zero. This conclusion is inconsistent with Nernst theorem. In the extreme case r
+
/
c
2
=
r
0
2, the effective temperature from (15) is
(18)
T
eff
=
1
12
π
r
0
(
1
-
5
Q
2
2
r
0
2
)
.
The effective pressure is
(19)
P
eff
=
0
.
In this case the volume-thermodynamic system becomes area-thermodynamic one. According to (19) the pressure of thermodynamic membrane is zero. However from (18), the temperature of thermodynamic membrane is nonzero. This can partly solve the problem that extreme de Sitter black holes do not satisfy the Nernst theorem, when Q
=
0, (15) and (16) return to the known result [34].


## 4. Critical Behaviour

To compare with the van der Waals equation, we setP
eff
→
P, v
→
v and discuss the phase transition and the critical phenomena when r
c is invariant. The van der Waals equation is
(20)
(
P
+
a
v
2
)
(
v
-
b
~
)
=
k
T
.
Here, v
=
V
/
N is the specific volume of the fluid, P is its pressure, T is its temperature, and k is the Boltzmann constant.Substituting (15) into (16), we obtain
(21)
P
eff
=
T
eff
B
4
2
r
c
B
2
+
B
2
B
3
-
B
1
B
4
8
π
r
c
2
x
(
1
+
x
)
B
2
,
where
(22)
B
1
=
1
+
x
-
2
x
2
+
x
3
+
x
4
1
+
x
+
x
2
,
B
2
=
1
+
x
+
x
2
-
2
x
3
+
x
4
+
x
5
+
x
6
1
+
x
+
x
2
,
B
3
=
1
+
2
x
-
2
x
4
-
x
5
(
1
+
x
+
x
2
)
2
,
B
4
=
1
+
2
x
+
3
x
2
-
3
x
5
-
2
x
6
-
x
7
(
1
+
x
+
x
2
)
2
.According to (21), combing dimensional analysis [22] with (12), we conclude that we should identify the specific volume v with
(23)
v
=
r
c
(
1
-
x
)
.
From the two equations
(24)
∂
P
eff
∂
v
=
0
,
∂
2
P
eff
∂
v
2
=
0
,
we first calculate the position of critical points. Then, one can derive
(25)
(
∂
P
eff
∂
v
)
T
eff
=
-
1
×
(
8
π
r
c
5
(
1
+
x
)
(
1
+
x
+
x
2
)
3
000000
×
(
1
+
x
+
x
2
-
2
x
3
+
x
4
+
x
5
+
x
6
)
(
1
+
x
+
x
2
)
3
)
-
1
×
[
r
c
2
x
2
(
-
6
-
21
x
-
38
x
2
-
45
x
3
-
30
x
4
-
10
x
5
00000000
+
6
x
6
+
7
x
7
+
4
x
8
+
x
9
)
×
Q
2
x
(
15
+
54
x
+
98
x
2
+
104
x
3
+
59
x
4
+
18
x
5
000000000
-
9
x
6
-
12
x
7
-
10
x
8
-
4
x
9
-
x
10
)
]
=
0
(
∂
2
P
eff
∂
v
2
)
T
eff
=
1
×
(
4
π
r
c
6
(
1
+
x
)
(
1
+
x
+
x
2
)
4
0000
×
(
1
+
x
+
x
2
-
2
x
3
+
x
4
+
x
5
+
x
6
)
2
)
-
1
×
[
-
r
c
2
x
(
6
+
36
x
+
115
x
2
+
286
x
3
+
486
x
4
+
530
x
5
+
203
x
6
-
357
x
7
-
783
x
8
-
854
x
9
-
666
x
10
-
375
x
11
-
127
x
12
+
3
x
13
+
32
x
14
+
18
x
15
+
6
x
16
+
x
17
)
+
Q
2
(
30
+
165
x
+
456
x
2
+
837
x
3
+
1050
x
4
+
903
x
5
+
255
x
6
-
720
x
7
-
1707
x
8
-
2113
x
9
-
1743
x
10
-
969
x
11
-
314
x
12
-
9
x
13
+
63
x
14
+
44
x
15
+
21
x
16
+
6
x
17
+
x
18
)
]
=
0
.Whenr
c
=
1, from (15), (16), and (25) one can obtain the position of critical point
(26)
x
c
=
0.871992
.
The critical electric charge, specific volume, temperature, and the critical pressure are, respectively,
(27)
Q
c
=
0.60395
,
v
c
=
0.128008
,
T
c
=
0.00436559
,
p
c
=
0.0000145468
.In Figure1 we give the figure of P
eff with the change of v at the constant effective temperature near the critical point.Figure 1
P
eff
-
v diagram of RN-dS black holes. The temperature of isotherms decreases from top to bottom and corresponds to T
c
+
0.004, T
c
+
0.002, T
c, T
c
-
0.002.To reflect the influence ofr
c on the spacetime, we set r
c
=
5, from which we derived the position of the critical point
(28)
x
c
=
0.871992
.
The critical electric charge, specific volume, temperature, and the critical pressure are, respectively,
(29)
Q
c
=
3.01975
,
v
c
=
0.640038
,
T
c
=
0.000873119
,
p
c
=
5.8187
×
1
0
-
7
.
The diagram of the effective P
eff with the change of v is depicted in Figure 2.Figure 2
P
eff
-
v diagram of RN-dS black holes. The temperature of isotherms decreases from top to bottom and corresponds to T
c
+
0.00004, T
c
+
0.00002, T
c, T
c
-
0.00002.For the van der Waals fluid and the RN-AdS black hole, the relationP
c
v
c
/
T
c is a universal number and is independent of the charge Q. For the RN-dS black hole, according to the effective thermodynamic quantities, numerical calculation shows that P
c
v
c
/
T
c still has a Q-independent universal value. Certainly, the universal value is no more than 3
/
8, but ~
0.0004265.


## 5. Discussion and Conclusions

From above we can find out that the value ofr
c does not influence the critical point x; namely, for the RN-dS spacetime, the position of critical point is irrelevant to the value of the cosmological horizon. This indicates that x
=
r
c
/
r
+ is fixed; however the critical effective temperature, critical volume, and critical pressure are dependent on the value of r
c. The critical effective temperature and pressure for the RN-dS system will decrease as the values of r
c increase, while the critical electric charge and the critical volume will increase as the values of r
c increase.By Figures1 and 2, the P
eff
-
v curve at constant temperature of RN-dS spacetime is different from the ones of van der Waals equation and charged AdS black holes.(1)
The first difference lies at the critical pressureP
eff of RN-dS spacetime which increases as the volume increases at the constant temperature when T
eff
>
T
c, and the maximal value turns up at x
→
0, namely, de Sitter spacetime.
(2)
The first difference is that the critical pressureP
eff of RN-dS spacetime may be negative at the constant temperature when T
eff
<
T
c, which means the system is not stable. From (15) and (16) we can obtain the parameters x and Q when the system is in the unstable state.
(3)
On theP
eff
-
v curves with T
eff
>
T
c the system lies in a phase; on the P
eff
-
v curves with T
eff
<
T
c the same pressure will correspond to two different values of x, namely, two-phase coexistence region. Using the equal area criterion we can find out the proportion of the two phases for the RN-dS system.From the above discussion, in RN-dS spacetime when considering the relation between the two horizons there is the similar phase transition like the one in van der Waals equation and charged AdS black holes. The reason is still unclear. This deserves further study. If the cosmological constant is just the dark energy, the universe will evolve into a new de Sitter phase. According to Figures1 and 2 the RN-dS system can evolve into de Sitter phase along isothermal curve. However, along the different isothermal curves, which processes will be the evolution of the universe to a new de Sitter phase needs further consideration according to the observations.



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*Source: 124854-2014-03-10.xml*