# Vacuum Expectation Value Profiles of the Bulk Scalar Field in the Generalized Randall-Sundrum Model

Authors: A. Tofighi; M. Moazzen; A. Farokhtabar
Journal: Advances in High Energy Physics
 (2015)

---

## Abstract

In the generalized Randall-Sundrum warped brane-world model the
cosmological constant induced on the visible brane can be positive
or negative. In this paper we investigate profiles of vacuum
expectation value of the bulk scalar field under general Dirichlet
and Neumann boundary conditions in the generalized warped brane-world model. We show that the VEV profiles generally depend on the value
of the brane cosmological constant. We find that the VEV profiles of
the bulk scalar field for a visible brane with negative cosmological
constant and positive tension are quite distinct from those of
Randall-Sundrum model. In addition we show that the VEV profiles for
a visible brane with large positive cosmological constant are also
different from those of the Randall-Sundrum
model. We also verify that Goldberger and Wise mechanism can work under nonzero Dirichlet
boundary conditions in the generalized Randall-Sundrum model.


---

## Body

## 1. Introduction

Extra dimension is an important subject in the realm of theoretical physics that provides many creative ways to solve some problems in physics such as hierarchy problem. Unlike the model of Arkani-Hamed et al. [1], Randall and Sundrum (RS) proposed an alternative scenario [2] to solve the hierarchy problem that does not require large extra dimensions. They assumed an exponential function of the compactification radius called a warp factor in a 5-dimensional anti-de Sitter space-time compactified on a S
1
/
Z
2 orbifold. Two 3-branes are located at the orbifold fixed point ϕ
=
π (visible brane) and ϕ
=
0 (hidden brane). Due to the nonfactorizable geometry of metric all fundamental scalar masses are subject to an exponential suppression on the visible brane.In the original RS model the cosmological constant induced on the visible brane is zero and the brane tension is negative. This model has been generalized such that the cosmological constant on the brane as well as brane tension can be positive or negative [3]. In the RS model the size of extra dimension, r
c, is not determined by the dynamic of the model. For this scenario to be relevant, it is necessary to find a mechanism for generating a potential to stabilize the value of r
c. This mechanism was proposed by Goldberger and Wise (GW) [4] so that the dynamic of a five-dimensional bulk scalar field in such model could stabilize the size of extra dimension. In the GW mechanism the potential for the radion that sets the size of the fifth dimension is generated by a bulk scalar with quartic interactions localized on the two 3-branes. The minimum of this potential yields a compactification scale that solves the hierarchy problem without fine-tuning of parameters. The backreaction of the bulk scalar field was neglected in the original GW mechanism but it was studied in [5] later. Some studies about this mechanism can be found in [6–8].Recently, GW mechanism of radius stabilization in the brane-world model with nonzero brane cosmological constant has been considered [9]. It was shown that, for a generalized RS model, the modulus stabilization condition explicitly depends on the brane cosmological constant. Furthermore Haba et al. [10] have analyzed profiles of vacuum expectation value (VEV) of the bulk scalar field under the general boundary conditions (BCs) on the RS warped compactification. They have investigated GW mechanism in several setups with the general BCs of the bulk scalar field. Also they showed that S
U
(
2
)
R triplet Higgs in the bulk left-right symmetric model with custodial symmetry can be identified by the Goldberger-Wise scalar.The motivation for the present study is to study the VEV profile of the scalar field, including a brane cosmological constant and with different combinations of Dirichlet and Neumann boundary conditions at the two branes. We also want to know if this scalar can stabilize the size of the warped extra dimension. We note that the present accelerating phase of the universe is due to the presence of small positive cosmological constant with a tiny value of1
0
-
124 in Planck unit. Hence it is desirable to consider the effect of nonzero cosmological constant on the brane.This paper is organized as follows. In Section2, we briefly summarize the brane-world model with nonzero brane cosmological constant. In Section 3 we study the behavior of the bulk scalar field under four BCs on the general RS warped model in the case without brane localized potential and in the next section we analyze profiles of VEV of the bulk scalar field in the case with brane localized scalar potential. Also we investigate the GW mechanism under the BCs in the generalized brane-world scenario. Finally in Section 5 we conclude with the summary of our results.


## 2. The Generalized Randall-Sundrum Model

One of the many different possibilities that can be explored to solve the hierarchy problem is Randall-Sundrum (RS) model [2]. The RS model proposes that space-time is described by a 5D anti-de Sitter (AdS) metric. Some good reviews on this subject can be found in, for example, [11–13]. In the Randall-Sundrum model the visible brane tension is negative and the cosmological constant on the visible brane is assumed to be zero. It has been shown in [3] that one can indeed generalize the model with nonzero cosmological constant on the brane and still can have Planck to TeV scale warping from the resulting warp factor. In this section we want to study the warped brane-world model with nonzero brane cosmological constant briefly. Other studies for this model have been reported in [14–16].The action of a bulk scalar field,Φ, on the warp brane-world model that was suggested by Randall and Sundrum is(1)
S
=
∫
‍
d
5
x
-
G
-
G
M
N
∂
M
Φ
†
∂
N
Φ
-
V
,where x
M
=
(
x
μ
,
y
), μ
=
0,1
,
2,3. The general form of the warped metric for a five-dimensional space-time is given by(2)
G
M
N
d
x
M
d
x
N
=
e
-
2
A
(
y
)
g
μ
ν
d
x
μ
d
x
ν
+
d
y
2
,where g
μ
ν stands for four-dimensional curved brane. The brane tension k is defined by(3)
k
≡
±
-
Λ
6
M
5
3
=
V
U
V
6
M
5
3
=
-
V
I
R
6
M
5
3
,where M
5 is the Planck mass in five dimensions. We assume that the scalar field Φ is a function of the extra dimension y only that can be defined as [10](4)
Φ
=
Φ
R
+
i
Φ
I
2
,and, for simplicity, we take the bulk potential as(5)
V
=
m
2
Φ
2
=
m
2
2
(
Φ
R
2
+
Φ
I
2
)
.A scalar mass on the visible brane gets warped through the warp factor e
-
A
(
k
r
π
)
=
1
0
-
n where the warp factor index, n, is set to 16 to achieve the desired warping from Planck to TeV scale. The magnitude of the induced cosmological constant on the brane in the generalized RS model is nonvanishing and is given by 1
0
-
ℵ in Planck unit. For the negative value of the cosmological constant, Ω
<
0, on the visible brane which leads to AdS-Schwarzschild space-times the solution of the warp factor can be written as [9](6)
e
-
A
(
y
)
=
ω
cosh
⁡
(
ln
⁡
ω
c
1
+
k
y
)
,where ω
2
≡
-
Ω
/
3
k
2
≥
0 and c
1
=
1
+
1
-
ω
2. It was shown that real solution for the warp factor exists if and only if ω
2
≤
1
0
-
2
n. This leads to an upper bound for the magnitude of the cosmological constant as ℵ
=
2
n. When ℵ
=
ℵ
min
⁡
=
2
n, the visible brane tension is zero. For AdS brane, there are degenerate solutions of k
r
π whose values will depend on ω
2 and n. The brane tension is negative for some of these solutions and is positive for others. Next, for AdS brane we want to investigate the solution of the equation of motion which is obtained from the action given by (1). As it has been discussed in [3], to resolve the gauge hierarchy problem without introducing any intermediate scale, the brane cosmological constant should be tuned to a very small value; therefore in this case the warp factor in (6) can be given by [9](7)
e
-
4
A
(
y
)
=
e
-
4
k
y
+
ω
2
e
-
2
k
y
.We use background field method to study behaviors of the bulk scalar field of the generalized Randall-Sundrum model. In this method one separates the field into classical and quantum fluctuation parts. The configuration of the classical field obeys an equation of motion [10].With the above warp factor equation of motion for the classical field can be written down:(8)
∂
y
2
Φ
X
-
(
4
k
-
2
k
ω
2
e
2
k
y
)
∂
y
Φ
X
-
m
2
Φ
X
=
0
,where X stands for R and I. We solve the above equation and obtain the solution for the scalar field as(9)
Φ
X
(
z
)
=
A
z
ν
+
2
+
B
z
-
(
ν
-
2
)
+
α
A
z
ν
+
4
+
β
B
z
-
(
ν
-
4
)
,where(10)
α
=
-
ω
2
2
ν
+
2
ν
+
1
,
β
=
-
ω
2
2
2
-
ν
1
-
ν
,and ν
=
4
+
m
2
/
k
2 and z
=
e
k
y. In the above solution A and B are arbitrary constant which are evaluated by using the appropriate boundary conditions at the locations of the brane.For the positive induced brane cosmological constantΩ
>
0 which corresponds to dS-Schwarzschild space-time the warp factor turns out to be(11)
e
-
A
(
y
)
=
ω
sinh
⁡
(
ln
⁡
c
2
ω
-
k
y
)
,where ω
2
≡
Ω
/
3
k
2
≥
0 and c
2
=
1
+
1
+
ω
2. In this case there is no bound on the value of ω
2, and the positive cosmological constant can be of arbitrary magnitude. For dS brane, the brane tension is negative for the entire range of values of the positive cosmological constant. Also for a small ω the warp factor can be written down:(12)
e
-
4
A
(
y
)
=
e
-
4
k
y
-
ω
2
e
-
2
k
y
.By using the above warp factor the solution of the equation of motion for the dS brane is(13)
Φ
X
(
z
)
=
A
z
ν
+
2
+
B
z
-
(
ν
-
2
)
-
α
A
z
ν
+
4
-
β
B
z
-
(
ν
-
4
)
.It is obvious that by taking α
→
-
α and β
→
-
β we can obtain the above solution from AdS one. Notice that from now on we will use ω
2 to represent induced brane cosmological constant. With this generalized RS warped model we now investigate the profile of the bulk scalar field under boundary conditions in the next section.


## 3. VEV Profiles in the Absence of Brane Localized Potential

In this section, we study the VEV profiles of the bulk scalar field in a case without brane localized scalar potential in the generalized Randall-Sundrum model. By utilizing (2), the action can be rewritten as(14)
S
=
∫
‍
d
4
x
∫
0
L
‍
d
y
e
-
4
A
(
y
)
-
e
2
A
y
∂
μ
Φ
2
-
∂
y
Φ
2
-
V
.The above action was defined on a line segment as 0
≤
y
≤
L. If we write the bulk scalar as (4) then the variation of the action is given by(15)
δ
S
=
∫
‍
d
4
x
∫
0
L
‍
d
y
e
-
4
A
(
y
)
·
δ
Φ
X
ρ
Φ
X
-
∂
V
∂
Φ
X
g
g
ρ
Φ
X
-
∂
V
∂
Φ
X
+
δ
y
δ
Φ
X
+
∂
y
Φ
X
+
δ
y
-
L
δ
Φ
X
-
∂
y
Φ
X
,where ρ
=
e
2
A
(
y
)
□
+
e
4
A
(
y
)
∂
y
e
-
4
A
(
y
)
∂
y. The VEV profile is obtained by the action principal δ
S
=
0; that is,(16)
ρ
Φ
X
-
∂
V
∂
Φ
X
=
0
.Notice that the above equation of motion has been solved in the previous section for dS and AdS brane in (9) and (13), respectively. The boundary conditions at y
=
0 and L read as either Dirichlet(17)
δ
Φ
X
y
=
0
,
L
=
0or Neumann(18)
±
∂
y
Φ
X
y
=
0
,
L
=
0
,where plus and minus signs are for y
=
0 and y
=
L, respectively. As mentioned in [10] we can have four choices of combination of Dirichlet and Neumann boundary conditions shown by (
D
,
D
), (
D
,
N
), (
N
,
D
), and (
N
,
N
) at y
=
0 and L. Here by using the solution of the equation of motion that was given by (9) and (13) we want to verify the profile of the bulk scalar field under the four boundary conditions in the generalized Randall-Sundrum model with nonzero brane cosmological constant.


### 3.1.(
D
,
D
) Case

We discuss a case in which both boundary conditions on they
=
0 and y
=
L branes are the Dirichlet type boundary conditions. The most general form of the Dirichlet BC is δ
Φ
|
z
=
ξ
=
0 and(19)
υ
1
=
υ
1
,
υ
(
z
L
)
=
υ
2
,where ξ is taken as 1 and z
L
=
e
k
L. For AdS brane these boundary conditions can be rewritten by (9) as(20)
A
1
+
α
+
B
1
+
β
=
υ
1
,
A
z
L
ν
+
2
(
1
+
α
z
L
2
)
+
B
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
=
υ
2
.The above equations lead to(21)
A
=
-
υ
1
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
-
υ
2
(
1
+
β
)
z
L
(
ν
+
2
)
(
1
+
α
z
L
2
)
(
1
+
β
)
-
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
(
1
+
α
)
,
B
=
υ
1
z
L
(
ν
+
2
)
(
1
+
α
z
L
2
)
-
υ
2
(
1
+
α
)
z
L
(
ν
+
2
)
(
1
+
α
z
L
2
)
(
1
+
β
)
-
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
(
1
+
α
)
.Therefore, under (
D
,
D
) boundary conditions, in the generalized RS model with negative brane cosmological constant the VEV profile is(22)
υ
(
z
)
=
-
υ
1
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
-
υ
2
(
1
+
β
)
z
L
(
ν
+
2
)
(
1
+
α
z
L
2
)
(
1
+
β
)
-
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
(
1
+
α
)
z
ν
+
2
+
υ
1
z
L
(
ν
+
2
)
(
1
+
α
z
L
2
)
-
υ
2
(
1
+
α
)
z
L
(
ν
+
2
)
(
1
+
α
z
L
2
)
(
1
+
β
)
-
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
(
1
+
α
)
z
-
ν
+
2
-
α
υ
1
z
L
-
ν
+
2
1
+
β
z
L
2
-
υ
2
1
+
β
z
L
ν
+
2
1
+
α
z
L
2
1
+
β
-
z
L
-
ν
+
2
1
+
β
z
L
2
1
+
α
·
z
ν
+
4
+
β
υ
1
z
L
ν
+
2
1
+
α
z
L
2
-
υ
2
1
+
α
z
L
ν
+
2
1
+
α
z
L
2
1
+
β
-
z
L
-
ν
+
2
1
+
β
z
L
2
1
+
α
·
z
-
ν
+
4
;notice that for ω
=
0 (i.e., the RS case) which corresponds to α
=
0 and β
=
0 the above equations lead to the results that were proposed by Haba et al. [10] for (
D
,
D
) BCs.In Figure1 the VEV profile for ℵ
=
34 is shown for the AdS brane. In this figure we have assumed the brane tension of visible brane to be positive (see (A.4) for details). we find that the pattern of localization is different from that of the RS case. It is seen that the position of the IR brane shifts to the larger value of z
L so the drastic change of the VEV profile occurs later than RS case. For this figure we have taken υ
≡
υ
0,1
,
2
,
L
≡
M
p
l
3
/
2, k
≡
M
p
l, ν
=
2.1, M
p
l
=
2.4
×
1
0
18 GeV.Figure 1
The VEV profile under(
D
,
D
) BCs as a function of extra dimension for ℵ
=
34 in the absence of brane potential with Ω
<
0 and a positive tension visible brane. We take υ
≡
υ
0,1
,
2
,
L
≡
M
p
l
3
/
2, k
≡
M
p
l, ν
=
2.1, M
p
l
=
2.4
×
1
0
18 GeV.For dS brane,α
→
-
α and β
→
-
β; therefore A and B can be written as(23)
A
=
-
υ
1
z
L
(
-
ν
+
2
)
(
1
-
β
z
L
2
)
-
υ
2
(
1
-
β
)
z
L
(
ν
+
2
)
(
1
-
α
z
L
2
)
(
1
-
β
)
-
z
L
(
-
ν
+
2
)
(
1
-
β
z
L
2
)
(
1
-
α
)
,
B
=
υ
1
z
L
(
ν
+
2
)
(
1
-
α
z
L
2
)
-
υ
2
(
1
-
α
)
z
L
(
ν
+
2
)
(
1
-
α
z
L
2
)
(
1
-
β
)
-
z
L
(
-
ν
+
2
)
(
1
-
β
z
L
2
)
(
1
-
α
)
.By utilizing the above form of A and B in (13) the VEV profile of bulk scalar field is obtained for dS brane. We investigate this VEV profile for large and small values of ω. We find that for the small values of positive brane cosmological constant the VEV profile has tiny difference with respect to the RS case.In Figure2, we show the results for the large positive brane cosmological constant, namely, ℵ
=
20 (dotted line) and ℵ
=
28 (dashed line). For the sake of comparison we also include ℵ
=
∞ (solid line, i.e., RS case). It is observed that the profile localizes near the IR brane. But the location of the IR brane is different in comparison to the RS case (see (A.7) of the Appendix).Figure 2
The dependence of VEV profile under(
D
,
D
) BCs for large positive brane cosmological constant with ℵ
=
20 (dotted line), ℵ
=
28 (dashed line), and ℵ
=
∞ (solid line, i.e., RS case). We take the same values for other parameters as the ones in Figure 1.In(
D
,
N
) case, the boundary conditions can be given by(24)
υ
(
1
)
=
υ
1
,
∂
z
υ
z
z
=
z
L
=
0
.Then, for AdS brane they are written down as(25)
A
(
1
+
α
)
+
B
(
1
+
β
)
=
υ
1
,
A
z
L
ν
+
2
(
v
+
2
+
α
(
ν
+
4
)
z
L
2
)
-
B
z
L
-
(
ν
-
2
)
(
ν
-
2
+
β
(
ν
-
4
)
z
L
2
)
=
0
.These lead to(26)
A
=
υ
1
z
L
-
ν
+
2
ν
-
2
+
β
z
L
2
ν
-
4
·
z
L
(
-
ν
+
2
)
(
1
+
α
)
[
(
ν
-
2
)
+
β
z
L
2
(
ν
-
4
)
]
d
d
d
+
z
L
ν
+
2
1
+
β
ν
+
2
+
α
z
L
2
ν
+
4
-
1
,
B
=
υ
1
z
L
ν
+
2
ν
+
2
+
α
z
L
2
ν
+
4
·
z
L
(
-
ν
+
2
)
(
1
+
α
)
[
(
ν
-
2
)
+
β
z
L
2
(
ν
-
4
)
]
d
d
d
+
z
L
ν
+
2
1
+
β
ν
+
2
+
α
z
L
2
ν
+
4
-
1
.By substituting the above form of A and B in (9) the VEV profile in (
D
,
N
) case of boundary conditions is obtained.


### 3.2.(
N
,
D
) Case

Next, we consider the(
N
,
D
) case. These boundary conditions can be described by(27)
∂
z
υ
z
z
=
1
=
0
,
υ
(
z
L
)
=
υ
2
.For negative brane cosmological constant, they are(28)
A
(
ν
+
2
+
α
(
ν
+
4
)
)
-
B
(
ν
-
2
+
β
(
ν
-
4
)
)
=
0
,
A
z
L
ν
+
2
(
1
+
α
z
L
2
)
+
B
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
=
υ
2
.These lead to(29)
A
=
υ
2
[
(
ν
-
2
)
+
β
(
ν
-
4
)
]
·
z
L
-
ν
+
2
1
+
β
z
L
2
ν
+
2
+
α
ν
+
4
d
d
d
+
z
L
ν
+
2
1
+
α
z
L
2
ν
-
2
+
β
ν
-
4
-
1
,
B
=
υ
2
[
(
ν
+
2
)
+
α
(
ν
+
4
)
]
·
z
L
-
ν
+
2
1
+
β
z
L
2
ν
+
2
+
α
ν
+
4
f
f
f
+
z
L
ν
+
2
1
+
α
z
L
2
ν
-
2
+
β
ν
-
4
-
1
.Like the previous subsection we substitute the above form of A and B into (9) to obtain the VEV profile in (
N
,
D
) case of boundary conditions.


### 3.3.(
N
,
N
) Case

Finally, we investigate the(
N
,
N
) case. These boundary conditions are(30)
∂
z
υ
z
z
=
1
=
0
,
∂
z
υ
z
z
=
z
L
=
0
.Then, for AdS brane they are written down as(31)
A
ν
+
2
+
α
ν
+
4
-
B
ν
-
2
+
β
ν
-
4
=
0
,
A
z
L
ν
+
2
ν
+
2
+
α
ν
+
4
z
L
2
-
B
z
L
-
ν
-
2
ν
-
2
+
β
ν
-
4
z
L
2
=
0
.We find that like RS model there is no solution to satisfy the above boundary conditions except for a trivial one, (
A
,
B
)
=
(
0,0
), which is not of physical interest.In this section we studied the VEV profile of a bulk scalar field under four boundary conditions on a generalized warped brane-world model in the absence of brane localized potential. We found that the VEV profiles depend on the vanishingly small brane cosmological constant.


## 3.1.(
D
,
D
) Case

We discuss a case in which both boundary conditions on they
=
0 and y
=
L branes are the Dirichlet type boundary conditions. The most general form of the Dirichlet BC is δ
Φ
|
z
=
ξ
=
0 and(19)
υ
1
=
υ
1
,
υ
(
z
L
)
=
υ
2
,where ξ is taken as 1 and z
L
=
e
k
L. For AdS brane these boundary conditions can be rewritten by (9) as(20)
A
1
+
α
+
B
1
+
β
=
υ
1
,
A
z
L
ν
+
2
(
1
+
α
z
L
2
)
+
B
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
=
υ
2
.The above equations lead to(21)
A
=
-
υ
1
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
-
υ
2
(
1
+
β
)
z
L
(
ν
+
2
)
(
1
+
α
z
L
2
)
(
1
+
β
)
-
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
(
1
+
α
)
,
B
=
υ
1
z
L
(
ν
+
2
)
(
1
+
α
z
L
2
)
-
υ
2
(
1
+
α
)
z
L
(
ν
+
2
)
(
1
+
α
z
L
2
)
(
1
+
β
)
-
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
(
1
+
α
)
.Therefore, under (
D
,
D
) boundary conditions, in the generalized RS model with negative brane cosmological constant the VEV profile is(22)
υ
(
z
)
=
-
υ
1
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
-
υ
2
(
1
+
β
)
z
L
(
ν
+
2
)
(
1
+
α
z
L
2
)
(
1
+
β
)
-
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
(
1
+
α
)
z
ν
+
2
+
υ
1
z
L
(
ν
+
2
)
(
1
+
α
z
L
2
)
-
υ
2
(
1
+
α
)
z
L
(
ν
+
2
)
(
1
+
α
z
L
2
)
(
1
+
β
)
-
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
(
1
+
α
)
z
-
ν
+
2
-
α
υ
1
z
L
-
ν
+
2
1
+
β
z
L
2
-
υ
2
1
+
β
z
L
ν
+
2
1
+
α
z
L
2
1
+
β
-
z
L
-
ν
+
2
1
+
β
z
L
2
1
+
α
·
z
ν
+
4
+
β
υ
1
z
L
ν
+
2
1
+
α
z
L
2
-
υ
2
1
+
α
z
L
ν
+
2
1
+
α
z
L
2
1
+
β
-
z
L
-
ν
+
2
1
+
β
z
L
2
1
+
α
·
z
-
ν
+
4
;notice that for ω
=
0 (i.e., the RS case) which corresponds to α
=
0 and β
=
0 the above equations lead to the results that were proposed by Haba et al. [10] for (
D
,
D
) BCs.In Figure1 the VEV profile for ℵ
=
34 is shown for the AdS brane. In this figure we have assumed the brane tension of visible brane to be positive (see (A.4) for details). we find that the pattern of localization is different from that of the RS case. It is seen that the position of the IR brane shifts to the larger value of z
L so the drastic change of the VEV profile occurs later than RS case. For this figure we have taken υ
≡
υ
0,1
,
2
,
L
≡
M
p
l
3
/
2, k
≡
M
p
l, ν
=
2.1, M
p
l
=
2.4
×
1
0
18 GeV.Figure 1
The VEV profile under(
D
,
D
) BCs as a function of extra dimension for ℵ
=
34 in the absence of brane potential with Ω
<
0 and a positive tension visible brane. We take υ
≡
υ
0,1
,
2
,
L
≡
M
p
l
3
/
2, k
≡
M
p
l, ν
=
2.1, M
p
l
=
2.4
×
1
0
18 GeV.For dS brane,α
→
-
α and β
→
-
β; therefore A and B can be written as(23)
A
=
-
υ
1
z
L
(
-
ν
+
2
)
(
1
-
β
z
L
2
)
-
υ
2
(
1
-
β
)
z
L
(
ν
+
2
)
(
1
-
α
z
L
2
)
(
1
-
β
)
-
z
L
(
-
ν
+
2
)
(
1
-
β
z
L
2
)
(
1
-
α
)
,
B
=
υ
1
z
L
(
ν
+
2
)
(
1
-
α
z
L
2
)
-
υ
2
(
1
-
α
)
z
L
(
ν
+
2
)
(
1
-
α
z
L
2
)
(
1
-
β
)
-
z
L
(
-
ν
+
2
)
(
1
-
β
z
L
2
)
(
1
-
α
)
.By utilizing the above form of A and B in (13) the VEV profile of bulk scalar field is obtained for dS brane. We investigate this VEV profile for large and small values of ω. We find that for the small values of positive brane cosmological constant the VEV profile has tiny difference with respect to the RS case.In Figure2, we show the results for the large positive brane cosmological constant, namely, ℵ
=
20 (dotted line) and ℵ
=
28 (dashed line). For the sake of comparison we also include ℵ
=
∞ (solid line, i.e., RS case). It is observed that the profile localizes near the IR brane. But the location of the IR brane is different in comparison to the RS case (see (A.7) of the Appendix).Figure 2
The dependence of VEV profile under(
D
,
D
) BCs for large positive brane cosmological constant with ℵ
=
20 (dotted line), ℵ
=
28 (dashed line), and ℵ
=
∞ (solid line, i.e., RS case). We take the same values for other parameters as the ones in Figure 1.In(
D
,
N
) case, the boundary conditions can be given by(24)
υ
(
1
)
=
υ
1
,
∂
z
υ
z
z
=
z
L
=
0
.Then, for AdS brane they are written down as(25)
A
(
1
+
α
)
+
B
(
1
+
β
)
=
υ
1
,
A
z
L
ν
+
2
(
v
+
2
+
α
(
ν
+
4
)
z
L
2
)
-
B
z
L
-
(
ν
-
2
)
(
ν
-
2
+
β
(
ν
-
4
)
z
L
2
)
=
0
.These lead to(26)
A
=
υ
1
z
L
-
ν
+
2
ν
-
2
+
β
z
L
2
ν
-
4
·
z
L
(
-
ν
+
2
)
(
1
+
α
)
[
(
ν
-
2
)
+
β
z
L
2
(
ν
-
4
)
]
d
d
d
+
z
L
ν
+
2
1
+
β
ν
+
2
+
α
z
L
2
ν
+
4
-
1
,
B
=
υ
1
z
L
ν
+
2
ν
+
2
+
α
z
L
2
ν
+
4
·
z
L
(
-
ν
+
2
)
(
1
+
α
)
[
(
ν
-
2
)
+
β
z
L
2
(
ν
-
4
)
]
d
d
d
+
z
L
ν
+
2
1
+
β
ν
+
2
+
α
z
L
2
ν
+
4
-
1
.By substituting the above form of A and B in (9) the VEV profile in (
D
,
N
) case of boundary conditions is obtained.


## 3.2.(
N
,
D
) Case

Next, we consider the(
N
,
D
) case. These boundary conditions can be described by(27)
∂
z
υ
z
z
=
1
=
0
,
υ
(
z
L
)
=
υ
2
.For negative brane cosmological constant, they are(28)
A
(
ν
+
2
+
α
(
ν
+
4
)
)
-
B
(
ν
-
2
+
β
(
ν
-
4
)
)
=
0
,
A
z
L
ν
+
2
(
1
+
α
z
L
2
)
+
B
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
=
υ
2
.These lead to(29)
A
=
υ
2
[
(
ν
-
2
)
+
β
(
ν
-
4
)
]
·
z
L
-
ν
+
2
1
+
β
z
L
2
ν
+
2
+
α
ν
+
4
d
d
d
+
z
L
ν
+
2
1
+
α
z
L
2
ν
-
2
+
β
ν
-
4
-
1
,
B
=
υ
2
[
(
ν
+
2
)
+
α
(
ν
+
4
)
]
·
z
L
-
ν
+
2
1
+
β
z
L
2
ν
+
2
+
α
ν
+
4
f
f
f
+
z
L
ν
+
2
1
+
α
z
L
2
ν
-
2
+
β
ν
-
4
-
1
.Like the previous subsection we substitute the above form of A and B into (9) to obtain the VEV profile in (
N
,
D
) case of boundary conditions.


## 3.3.(
N
,
N
) Case

Finally, we investigate the(
N
,
N
) case. These boundary conditions are(30)
∂
z
υ
z
z
=
1
=
0
,
∂
z
υ
z
z
=
z
L
=
0
.Then, for AdS brane they are written down as(31)
A
ν
+
2
+
α
ν
+
4
-
B
ν
-
2
+
β
ν
-
4
=
0
,
A
z
L
ν
+
2
ν
+
2
+
α
ν
+
4
z
L
2
-
B
z
L
-
ν
-
2
ν
-
2
+
β
ν
-
4
z
L
2
=
0
.We find that like RS model there is no solution to satisfy the above boundary conditions except for a trivial one, (
A
,
B
)
=
(
0,0
), which is not of physical interest.In this section we studied the VEV profile of a bulk scalar field under four boundary conditions on a generalized warped brane-world model in the absence of brane localized potential. We found that the VEV profiles depend on the vanishingly small brane cosmological constant.


## 4. VEV Profiles in the Presence of Brane Localized Potentials

In this section, we formulate the VEV profiles of the bulk scalar field in a case with brane localized scalar potentials in the generalized Randall-Sundrum model. The action of a bulk field in the presence of brane potentials reads as(32)
S
=
∫
‍
d
4
x
∫
0
L
‍
d
y
e
-
4
A
(
y
)
·
-
e
2
A
y
∂
μ
Φ
2

-

∂
y
Φ
2

-

V
-
δ
y
V
0
-
δ
y
-
L
V
L
.The variation of the action is (33)
δ
S
=
∫
‍
d
4
x
∫
0
L
‍
d
y
e
-
4
A
(
y
)
·
δ
Φ
X
ρ
Φ
X
-
∂
V
∂
Φ
X
sss
+
δ
y
δ
Φ
X
+
∂
y
Φ
X
-
∂
V
0
∂
Φ
X
s
s
s
+
δ
y
-
L
δ
Φ
X
-
∂
y
Φ
X
-
∂
V
L
∂
Φ
X
.From the above equation the Dirichlet boundary condition is the same as (17) while the Neumann boundary condition should be modified as(34)
±
∂
y
Φ
X
-
∂
V
η
∂
Φ
X
y
=
η
=
0
,
L
=
0
.In this paper we seek to generalize the Randall-Sundrum model and moreover we want to investigate the GW mechanism. Therefore we use the brane potentials as [2, 4, 10](35)
V
η
=
λ
η
Φ
2
-
v
η
2
2
2
=
λ
η
4
Φ
R
2
+
Φ
I
2
-
v
η
2
2
,where λ
0 and λ
L stand for the brane tension and υ
0 and υ
L are the VEV of the bulk scalar field on the U
V and I
R brane, respectively. By utilizing the above scalar potentials we study the VEV profile in the case with brane localized potential in the generalized RS model. We notice that, like the RS model, the (
D
,
D
) boundary conditions in this case are the same as the ones for (
D
,
D
) case with brane potentials.For some other choices of the brane potentials see [8].


### 4.1.(
D
,
N
) Case

Here, we consider the(
D
,
N
) case that can be given by(36)
υ
(
1
)
=
υ
1
∂
z
υ
z
z
=
z
L
+
∂
V
L
∂
Φ
z
=
z
L
=
0
.For AdS brane these boundary conditions are written down as(37)
A
(
1
+
α
)
+
B
(
1
+
β
)
=
υ
1
,
(38)
k
A
z
L
ν
+
2
(
ν
+
2
+
α
(
ν
+
4
)
z
L
2
)
z
L
-
(
ν
-
2
)
s
s
s
-
B
z
L
-
(
ν
-
2
)
(
ν
-
2
+
β
(
ν
-
4
)
z
L
2
)
+
λ
L
A
z
L
ν
+
2
1
+
α
z
L
2
+
B
z
L
-
ν
+
2
1
+
β
z
L
2
·
[
A
z
L
ν
+
2
1
+
α
z
L
2
+
B
z
L
-
ν
+
2
1
+
β
z
L
2
2
-
υ
L
2
]
=
0
.We should remember that when the coupling in the boundary potential is infinite, the Neumann boundary conditions turn to Dirichlet one if we choose υ
L
=
υ
2.When the boundary quartic coupling is finite, the numerical calculation indicates thatA
≪
B
≃
z
L
ν
-
2
υ
L
(
1
-
β
z
L
2
) as a solution of (37) and (38). For the small boundary quartic coupling, A and B can be approximated by(39)
A
≃
χ
B
ν
-
2
+
β
z
L
2
ν
-
4
ν
+
2
+
α
z
L
2
ν
+
4
z
L
-
2
ν
,
B
≃
υ
L
2
+
k
1
-
χ
ν
-
2
+
β
z
L
2
ν
-
4
λ
L
(
1
+
β
z
L
2
)
z
L
ν
-
2
1
+
β
z
L
2
,where χ is determined by (37) and numerical calculation shows that χ
≃
O
(
1
) and χ
=
1 for λ
L
=
0. Also, χ is limited by(40)
χ
≤
1
+
λ
L
(
1
+
β
z
L
2
)
υ
L
2
k
[
ν
-
2
+
β
z
L
2
(
ν
-
4
)
]
.In Figure 3 we show the dependence of VEV profile for negative induced brane cosmological constant with positive brane tension with λ
~
L
=
100.Figure 3
The VEV profile for negative induced brane cosmological constant with positive brane tension forℵ
=
33 (dotted line), ℵ
=
34 (dashed line), and ℵ
=
∞ (solid line, i.e., RS case) in the (
D
,
N
) case for λ
~
L
=
100. The values of other parameters of the model are the same as the ones in Figure 1.


### 4.2.(
N
,
D
) Case

For the(
N
,
D
) case, these boundary conditions are given by(41)
∂
z
υ
z
z
=
1
-
∂
V
0
∂
Φ
z
=
1
=
0
,
∂
z
υ
z
z
=
z
L
=
0
.Then, for negative brane cosmological constant they are written down by (42)
k
[
A
ν
+
2
+
α
ν
+
4
-
B
ν
-
2
+
β
ν
-
4
]
-
λ
0
A
1
+
α
+
B
1
+
β
·
A
1
+
α
+
B
1
+
β
2
-
υ
0
2
=
0
,
A
z
L
ν
+
2
(
1
+
α
z
L
2
)
+
B
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
=
υ
2
.Numerical calculation indicates that A
~
B
~
υ
2
/
z
L
2
(
1
+
α
z
L
2
) and, for small λ
0, λ
~
0
≤
O
(
0.01
), A and B are approximated by(43)
A
≃
(
1
-
Γ
1
Γ
1
+
Γ
2
z
L
2
ν
)
υ
2
z
L
-
(
ν
+
2
)
1
+
α
z
L
2
,
B
≃
Γ
1
Γ
1
+
Γ
2
z
L
2
ν
υ
2
z
L
ν
-
2
1
+
β
z
L
2
,where(44)
Γ
1
=
(
1
+
β
z
L
2
)
[
k
(
ν
+
2
+
α
(
ν
+
4
)
)
+
λ
0
υ
0
2
(
1
+
α
)
]
,
Γ
2
=
(
1
+
α
z
L
2
)
[
k
(
ν
-
2
+
β
(
ν
-
4
)
)
-
λ
0
υ
0
2
(
1
+
β
)
]
.Figure 4 shows the VEV profile for large positive brane cosmological constant, when λ
~
0
=
100.Figure 4
The VEV profile for large positive brane cosmological constant withℵ
=
20 (dotted line), ℵ
=
28 (dashed line), and ℵ
=
∞ (solid line, i.e., RS case) in the (
N
,
D
) case for λ
~
0
=
100. The values of other parameters of the model are the same as the ones in Figure 1.


### 4.3.(
N
,
N
) Case

The(
N
,
N
) case of boundary conditions for AdS brane is(45)
∂
z
υ
z
z
=
1
-
∂
V
0
∂
Φ
z
=
1
=
0
,
∂
z
υ
z
z
=
L
+
∂
V
L
∂
Φ
z
=
L
=
0
.Then, the boundary conditions can be written down as (46)
k
A
ν
+
2
+
α
ν
+
4
-
B
ν
-
2
+
β
ν
-
4
-
λ
0
A
1
+
α
+
B
1
+
β
·
A
1
+
α
+
B
1
+
β
2
-
υ
0
2
=
0
,
k
A
z
L
ν
+
2
ν
+
2
+
α
ν
+
4
z
L
2
z
L
-
ν
-
2
s
s
s
-
B
z
L
-
ν
-
2
ν
-
2
+
β
ν
-
4
z
L
2
+
λ
L
A
z
L
ν
+
2
1
+
α
z
L
2
+
B
z
L
-
ν
+
2
1
+
β
z
L
2
·
A
z
L
ν
+
2
1
+
α
z
L
2
+
B
z
L
-
ν
+
2
1
+
β
z
L
2
2
-
υ
L
2
=
0
.In the limit of very small boundary couplings, λ
~
0
≪
O
(
0.01
) and λ
~
L
≪
O
(
0.1
), A and B are zero, but for large boundary quartic couplings which are considered in GW mechanism we have(47)
A
GW
≃
-
υ
0
(
1
+
β
z
L
2
)
Δ
1
z
L
-
2
ν
+
υ
L
(
1
+
β
)
Δ
1
z
L
-
(
ν
+
2
)
,
B
GW
≃
υ
0
1
+
α
z
L
2
Δ
1
1
+
Δ
2
Δ
1
z
L
-
2
ν
-
υ
L
1
+
α
Δ
1
z
L
-
ν
+
2
,where(48)
Δ
1
=
(
1
+
β
)
(
1
+
α
z
L
2
)
,
Δ
2
=
(
1
+
α
)
(
1
+
β
z
L
2
)
.Here we numerically analyze the VEV profile for finite boundary couplings. The result is shown in Figure 5 for large values of λ
~
0 and λ
~
L. At the end of this section we reconsider the realization of the GW mechanism under general boundary conditions in the generalized RS model. In the GW mechanism the effective potential for the modulus can be generated by the total action integral of a bulk scalar field with quartic interactions localized in two 3-branes. The bulk scalar field acts an important role to stabilize the radion which yields a compactification scale in terms of VEVs profile of the scalar field at two branes. The VEV of the bulk scalar can be obtained by solving the equation of motion.Figure 5
The VEV profile for negative induced brane cosmological constant with positive brane tension forℵ
=
33 (dotted line), ℵ
=
34 (dashed line), and ℵ
=
∞ (solid line, i.e., RS case) in the (
N
,
N
) case for λ
~
0
=
100, λ
~
L
=
100. The values of other parameters of the model are the same as the ones in Figure 1.Recently, this mechanism was studied in the generalized warped brane models with a nonzero brane cosmological constant by [9]. They have obtained the modulus stabilization condition for both positive and negative values of the brane cosmological constant.We have investigated the unknown coefficientsA and B of the VEV profile of the bulk scalar field in the generalized RS model by imposing boundary conditions which are given in Sections 3 and 4. It is well known that the (
N
,
N
) type boundary conditions given by (47) should be taken in the GW mechanism. The situation in the generalized warped model is similar to RS warped model as discussed in [10]. When the boundary quartic couplings λ
0 and λ
L are large the (
N
,
N
) BCs which were imposed in the GW mechanism are equivalent to (
D
,
D
) ones given in (20) if we take υ
1
=
υ
0 and υ
2
=
υ
L, so by this assumption in the limit of large boundary couplings, A and B given by (21) are A
≃
A
GW and B
≃
B
GW; therefore the GW mechanism can be realized in the (
D
,
D
) case with appropriate VEV profile.In the generalized warped model as mentioned in [10], when the brane localized potential is considered, GW mechanism can also work in (
N
,
D
) and (
D
,
N
) BCs with large boundary quartic couplings. The GW mechanism can not work when one of the boundary couplings λ
0 or λ
L becomes small in (
N
,
N
) case.


## 4.1.(
D
,
N
) Case

Here, we consider the(
D
,
N
) case that can be given by(36)
υ
(
1
)
=
υ
1
∂
z
υ
z
z
=
z
L
+
∂
V
L
∂
Φ
z
=
z
L
=
0
.For AdS brane these boundary conditions are written down as(37)
A
(
1
+
α
)
+
B
(
1
+
β
)
=
υ
1
,
(38)
k
A
z
L
ν
+
2
(
ν
+
2
+
α
(
ν
+
4
)
z
L
2
)
z
L
-
(
ν
-
2
)
s
s
s
-
B
z
L
-
(
ν
-
2
)
(
ν
-
2
+
β
(
ν
-
4
)
z
L
2
)
+
λ
L
A
z
L
ν
+
2
1
+
α
z
L
2
+
B
z
L
-
ν
+
2
1
+
β
z
L
2
·
[
A
z
L
ν
+
2
1
+
α
z
L
2
+
B
z
L
-
ν
+
2
1
+
β
z
L
2
2
-
υ
L
2
]
=
0
.We should remember that when the coupling in the boundary potential is infinite, the Neumann boundary conditions turn to Dirichlet one if we choose υ
L
=
υ
2.When the boundary quartic coupling is finite, the numerical calculation indicates thatA
≪
B
≃
z
L
ν
-
2
υ
L
(
1
-
β
z
L
2
) as a solution of (37) and (38). For the small boundary quartic coupling, A and B can be approximated by(39)
A
≃
χ
B
ν
-
2
+
β
z
L
2
ν
-
4
ν
+
2
+
α
z
L
2
ν
+
4
z
L
-
2
ν
,
B
≃
υ
L
2
+
k
1
-
χ
ν
-
2
+
β
z
L
2
ν
-
4
λ
L
(
1
+
β
z
L
2
)
z
L
ν
-
2
1
+
β
z
L
2
,where χ is determined by (37) and numerical calculation shows that χ
≃
O
(
1
) and χ
=
1 for λ
L
=
0. Also, χ is limited by(40)
χ
≤
1
+
λ
L
(
1
+
β
z
L
2
)
υ
L
2
k
[
ν
-
2
+
β
z
L
2
(
ν
-
4
)
]
.In Figure 3 we show the dependence of VEV profile for negative induced brane cosmological constant with positive brane tension with λ
~
L
=
100.Figure 3
The VEV profile for negative induced brane cosmological constant with positive brane tension forℵ
=
33 (dotted line), ℵ
=
34 (dashed line), and ℵ
=
∞ (solid line, i.e., RS case) in the (
D
,
N
) case for λ
~
L
=
100. The values of other parameters of the model are the same as the ones in Figure 1.


## 4.2.(
N
,
D
) Case

For the(
N
,
D
) case, these boundary conditions are given by(41)
∂
z
υ
z
z
=
1
-
∂
V
0
∂
Φ
z
=
1
=
0
,
∂
z
υ
z
z
=
z
L
=
0
.Then, for negative brane cosmological constant they are written down by (42)
k
[
A
ν
+
2
+
α
ν
+
4
-
B
ν
-
2
+
β
ν
-
4
]
-
λ
0
A
1
+
α
+
B
1
+
β
·
A
1
+
α
+
B
1
+
β
2
-
υ
0
2
=
0
,
A
z
L
ν
+
2
(
1
+
α
z
L
2
)
+
B
z
L
(
-
ν
+
2
)
(
1
+
β
z
L
2
)
=
υ
2
.Numerical calculation indicates that A
~
B
~
υ
2
/
z
L
2
(
1
+
α
z
L
2
) and, for small λ
0, λ
~
0
≤
O
(
0.01
), A and B are approximated by(43)
A
≃
(
1
-
Γ
1
Γ
1
+
Γ
2
z
L
2
ν
)
υ
2
z
L
-
(
ν
+
2
)
1
+
α
z
L
2
,
B
≃
Γ
1
Γ
1
+
Γ
2
z
L
2
ν
υ
2
z
L
ν
-
2
1
+
β
z
L
2
,where(44)
Γ
1
=
(
1
+
β
z
L
2
)
[
k
(
ν
+
2
+
α
(
ν
+
4
)
)
+
λ
0
υ
0
2
(
1
+
α
)
]
,
Γ
2
=
(
1
+
α
z
L
2
)
[
k
(
ν
-
2
+
β
(
ν
-
4
)
)
-
λ
0
υ
0
2
(
1
+
β
)
]
.Figure 4 shows the VEV profile for large positive brane cosmological constant, when λ
~
0
=
100.Figure 4
The VEV profile for large positive brane cosmological constant withℵ
=
20 (dotted line), ℵ
=
28 (dashed line), and ℵ
=
∞ (solid line, i.e., RS case) in the (
N
,
D
) case for λ
~
0
=
100. The values of other parameters of the model are the same as the ones in Figure 1.


## 4.3.(
N
,
N
) Case

The(
N
,
N
) case of boundary conditions for AdS brane is(45)
∂
z
υ
z
z
=
1
-
∂
V
0
∂
Φ
z
=
1
=
0
,
∂
z
υ
z
z
=
L
+
∂
V
L
∂
Φ
z
=
L
=
0
.Then, the boundary conditions can be written down as (46)
k
A
ν
+
2
+
α
ν
+
4
-
B
ν
-
2
+
β
ν
-
4
-
λ
0
A
1
+
α
+
B
1
+
β
·
A
1
+
α
+
B
1
+
β
2
-
υ
0
2
=
0
,
k
A
z
L
ν
+
2
ν
+
2
+
α
ν
+
4
z
L
2
z
L
-
ν
-
2
s
s
s
-
B
z
L
-
ν
-
2
ν
-
2
+
β
ν
-
4
z
L
2
+
λ
L
A
z
L
ν
+
2
1
+
α
z
L
2
+
B
z
L
-
ν
+
2
1
+
β
z
L
2
·
A
z
L
ν
+
2
1
+
α
z
L
2
+
B
z
L
-
ν
+
2
1
+
β
z
L
2
2
-
υ
L
2
=
0
.In the limit of very small boundary couplings, λ
~
0
≪
O
(
0.01
) and λ
~
L
≪
O
(
0.1
), A and B are zero, but for large boundary quartic couplings which are considered in GW mechanism we have(47)
A
GW
≃
-
υ
0
(
1
+
β
z
L
2
)
Δ
1
z
L
-
2
ν
+
υ
L
(
1
+
β
)
Δ
1
z
L
-
(
ν
+
2
)
,
B
GW
≃
υ
0
1
+
α
z
L
2
Δ
1
1
+
Δ
2
Δ
1
z
L
-
2
ν
-
υ
L
1
+
α
Δ
1
z
L
-
ν
+
2
,where(48)
Δ
1
=
(
1
+
β
)
(
1
+
α
z
L
2
)
,
Δ
2
=
(
1
+
α
)
(
1
+
β
z
L
2
)
.Here we numerically analyze the VEV profile for finite boundary couplings. The result is shown in Figure 5 for large values of λ
~
0 and λ
~
L. At the end of this section we reconsider the realization of the GW mechanism under general boundary conditions in the generalized RS model. In the GW mechanism the effective potential for the modulus can be generated by the total action integral of a bulk scalar field with quartic interactions localized in two 3-branes. The bulk scalar field acts an important role to stabilize the radion which yields a compactification scale in terms of VEVs profile of the scalar field at two branes. The VEV of the bulk scalar can be obtained by solving the equation of motion.Figure 5
The VEV profile for negative induced brane cosmological constant with positive brane tension forℵ
=
33 (dotted line), ℵ
=
34 (dashed line), and ℵ
=
∞ (solid line, i.e., RS case) in the (
N
,
N
) case for λ
~
0
=
100, λ
~
L
=
100. The values of other parameters of the model are the same as the ones in Figure 1.Recently, this mechanism was studied in the generalized warped brane models with a nonzero brane cosmological constant by [9]. They have obtained the modulus stabilization condition for both positive and negative values of the brane cosmological constant.We have investigated the unknown coefficientsA and B of the VEV profile of the bulk scalar field in the generalized RS model by imposing boundary conditions which are given in Sections 3 and 4. It is well known that the (
N
,
N
) type boundary conditions given by (47) should be taken in the GW mechanism. The situation in the generalized warped model is similar to RS warped model as discussed in [10]. When the boundary quartic couplings λ
0 and λ
L are large the (
N
,
N
) BCs which were imposed in the GW mechanism are equivalent to (
D
,
D
) ones given in (20) if we take υ
1
=
υ
0 and υ
2
=
υ
L, so by this assumption in the limit of large boundary couplings, A and B given by (21) are A
≃
A
GW and B
≃
B
GW; therefore the GW mechanism can be realized in the (
D
,
D
) case with appropriate VEV profile.In the generalized warped model as mentioned in [10], when the brane localized potential is considered, GW mechanism can also work in (
N
,
D
) and (
D
,
N
) BCs with large boundary quartic couplings. The GW mechanism can not work when one of the boundary couplings λ
0 or λ
L becomes small in (
N
,
N
) case.


## 5. Conclusions

In the RS model a negative tension visible brane is utilized to describe our Universe. However, such negative tension branes are unstable. Hence in this work we considered a generalized RS warped model.In this paper, we investigated a bulk scalar field under Dirichlet and Neumann boundary conditions in a generalized RS warped model with a nonzero cosmological constant on the brane. First we have obtained the profiles of VEV of the bulk scalar in the absence of brane localized potential for the negative and positive brane cosmological constant. We find the following.(1)
For an AdS visible brane with negative brane tension the results are similar to RS case.
(2)
However for an AdS visible brane with positive brane tension the results are different from the RS case. In this case the VEV profile undergoes sudden changes near the IR brane. Moreover we see that the IR brane is displaced from its RS location. The coefficientsA and B are functions of the length of the stabilized modulus. Hence the change of the length of the stabilized modulus modifies the shape of the VEV in comparison to the RS case.
(3)
For a dS visible brane the results for small values ofω
2 are not different from the RS case. But for larger values of ω
2 we have departures from the RS result.Next we have considered the VEV profiles under general boundary conditions in the presence of brane localized potential for nonzero brane cosmological constant. We find that to see drastic changes of the profile near the IR brane for an AdS visible brane with positive brane tension, boundary coupling must be large, λ
~
L
~
O
10.We have also verified GW mechanism in the generalized RS model with Dirichlet and Neumann boundary conditions. Analogous to RS model [10] the GW mechanism can work under nonzero Dirichlet BCs with appropriate VEVs in the generalized RS model. It will be interesting to use these results to study the Dirichlet Higgs as radion stabilizer in the generalized warped compactification.Our analysis of consistent boundary conditions is similar to that of Csáki et al. [17]. It is possible to extend this work by studying the behavior of the bulk scalar field on the warped five dimensions by utilizing the background field method, separating the field into classical and quantum fluctuation parts, and to investigate the phenomenological consequences of the profile of the scalar field [10].There are quantum corrections from Casimir effect and induced gravity on the brane. One requires that the brane-world metric be a solution of the quantum-corrected Einstein equations. For the RS model this issue has been addressed in [18, 19]. From (12) we see that in the generalized RS model A
(
y
)
=
k
|
y
| plus extra small term due to the curved branes. In the RS model the sum of brane tensions of two branes is zero. However in the generalized RS model this sum is not zero [3]. Hence the discussion of the issue of self-consistency is different from that of the RS model. However it is reasonable to expect that GRS is self-consistent for some specific values of the parameters of the model.In the analysis presented in this work we have ignored the backreaction of the scalar field on the space-time geometry. The stress tensor for the scalar field in the limit of large modulus can be obtained [4]. For the (
N
,
N
) case with large boundary coupling, we find that if v
0
2
Δ
1
2
/
M
5
3
≪
1, v
L
2
Δ
1
2
/
M
5
3
≪
1, and m
2
/
k
2
≪
1, then one can neglect the stress tensor for the scalar field in comparison to the stress tensor induced by the bulk cosmological constant. Furthermore the parameters of the bulk and brane potential are constrained by these inequalities.In this work our choices for the bulk and the brane potentials were those of [2]. Other choices for the bulk potential and brane potentials are possible. The potential for the GW scalar Φ in the bulk [20] has the general form of V
Φ
=
m
2
Φ
2
+
C
3
Φ
3
+
C
4
Φ
4
+
⋯. It would be interesting to study the VEV profiles of the bulk scalar field in such generalized warped models.In a previous work we studied the case of a scalar field nonminimally coupled to the Ricci curvature scalar [21]. The case of massless, conformally coupled scalar field is self-consistent after the inclusion of quantum corrections. Hence it will be of interest to consider massless, conformally coupled scalar field in the generalized RS framework.



---

*Source: 590980-2015-04-28.xml*