Comparing a Gauge-Invariant Formulation and a “Conventional Complete Gauge-Fixing Approach” for l = 0, 1 Mode Perturbations on the Schwarzschild Background Spacetime

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Comparing a Gauge-Invariant Formulation and a “Conventional Complete Gauge-Fixing Approach” for l = 0, 1 Mode Perturbations on the Schwarzschild Background Spacetime

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Kouji Nakamura^*

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Submitted:

29 September 2024

Posted:

30 September 2024

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Abstract

Comparison of the gauge-invariant formulation for l=0,1-mode perturbations on the Schwarzschild background spacetime proposed in [K. Nakamura, Class. Quantum Grav. 38 (2021), 145010.] and a “conventional complete gauge-fixing approach” in which we use the spherical harmonic functions Ylm as the scalar harmonics from the starting point is discussed. Although it is often said that “gauge-invariant formulations in general-relativistic perturbations are equivalent to complete gauge-fixing approaches,” as the result of this comparison, we conclude that the derived solutions through the proposed gauge-invariant formulation and those through a “conventional complete gauge-fixing approach” are different. It is pointed out that there is a case where the boundary conditions and initial conditions are restricted in a conventional complete gauge-fixing approach.

Keywords:

Subject: Physical Sciences - Theoretical Physics

1. Introduction

Through the ground-based gravitational-wave detectors [1,2,3,4], many events of gravitational waves, mainly from black hole-black hole coalescences, have now been detected. We are now at the stage where there is no doubt about the existence of gravitational waves due to their direct observations. One of the future directions of gravitational-wave astronomy will be a precise science through the statistics of many events. Toward further development of gravitational-wave science, the projects of future ground-based gravitational-wave detectors [5,6] are also progressing to achieve more sensitive detectors and some projects of space gravitational-wave antenna are also progressing [7,8,9,10]. Although there are many targets of these detectors, the Extreme-Mass-Ratio-Inspiral (EMRI), which is a source of gravitational waves from the motion of a stellar mass object around a supermassive black hole, is a promising target of the Laser Interferometer Space Antenna [7]. Since the mass ratio of this EMRI is very small, we can describe the gravitational waves from EMRIs through black hole perturbations [11]. Furthermore, the sophistication of higher-order black hole perturbation theories is required to support gravitational-wave physics as a precise science. The motivation of our series of papers, Refs. [12,13,14,15,16] and this paper, is in this theoretical sophistication of black hole perturbation theories toward higher-order perturbations.

Although realistic black holes have their angular momentum and we have to consider the perturbation theory of a Kerr black hole for direct applications to the EMRI, we may say that further sophistications are possible even in perturbation theories on the Schwarzschild background spacetime. From the pioneering works by Regge and Wheeler [17] and Zerilli [18,19], there have been many studies on the perturbations in the Schwarzschild background spacetime [20,21,22,23,24,25,26,27,28,29,30,31,32,33]. In these works, perturbations are decomposed through the spherical harmonics

Y_{l m}

because of the spherical symmetry of the background spacetime, and

l = 0, 1

modes should be separately treated. These modes correspond to the monopole and dipole perturbations. Due to these separate treatments, “gauge-invariant” treatments for

l = 0

and

l = 1

modes were unclear.

Owing to this situation, in the previous papers [12,13,14,15,16], we proposed the strategy of the gauge-invariant treatments of these

l = 0, 1

mode perturbations, which is declared as Proposal 2.1 in Sec. 2 of this paper below. One of the important premises of our gauge-invariant perturbations is the distinction between the first-kind gauge and the second-kind gauge. The first-kind gauge is essentially the choice of the coordinate system on the single manifold, and we often use this first-kind gauge when we predict or interpret the measurement results of experiments and observations. On the other hand, the second-kind gauge is the choice of the point identifications between the points on the physical spacetime

M_{ϵ}

and the background spacetime

M

. This second-kind gauge has nothing to do with our physical spacetime

M_{ϵ}

. Although this difference is extensively explained in the Part I paper [14], we also emphasize this difference in Sec. 2 of this paper. The proposal in the Part I paper [14] is a part of our developments of the general formulation of a higher-order gauge-invariant perturbation theory on a generic background spacetime toward unambiguous sophisticated nonlinear general-relativistic perturbation theories [34,35,36,37,38,39]. Although we have been applied this general framework to cosmological perturbations [40,41,42,43,44,45,46,47], we applied it to black hole perturbations in the series of papers, i.e., Refs. [12,13,14,15,16] and this paper. Even in cosmological perturbation theories, the same problem as the above

l = 0, 1

-mode problem exists as gauge-invariant treatments of homogeneous modes of perturbations. In this sense, we can expect that the proposal in the previous paper [14] will be a clue to the same problem in gauge-invariant perturbation theory on the generic background spacetime.

In the Part I paper [14], we also derived the linearized Einstein equations in a gauge-invariant manner following Proposal 2.1. Perturbations on the spherically symmetric background spacetime are classified into even- and odd-mode perturbations. In the same paper [14], we also gave the strategy to solve the odd-mode perturbations including

l = 0, 1

modes. Furthermore, we also derived the formal solutions for the

l = 0, 1

odd-mode perturbations to the linearized Einstein equations following Proposal 2.1. In the Part II paper [15], we gave the strategy to solve the even-mode perturbations including

l = 0, 1

modes, and we also derive the formal solutions for the

l = 0, 1

even-mode perturbations following Proposal 2.1. In the Part III paper [16], we find the fact that the derived solutions in the Part II paper [15] realize the linearized version of two exact solutions: one is the Lemaître-Tolman-Bondi (LTB) solution [48] and the other is the non-rotating C-metric [49,50]. Due to this fact, we conclude that the solutions for even-mode perturbations derived in the Part II paper [15] are physically reasonable. This series of papers is the full paper version of our short paper [12]. Furthermore, brief discussions on the extension to the higher-order perturbations are given in the short paper [13].

On the other hand, it is well-known the fact that we cannot construct gauge-invariant variables for

l = 0, 1

modes in a similar manner to

l \geq 2

modes if we decompose the metric perturbations through the spherical harmonics as the scalar harmonics from the starting point. For this reason, we usually use gauge-fixing approaches. Furthermore, it is often said that “gauge-invariant formulations in general-relativistic perturbations are equivalent to complete gauge-fixing approaches.” In this paper, we check this statement through the comparison of our proposed gauge-invariant formulation, in which we introduce singular harmonics at once and regularize them after the derivation of the mode-by-mode Einstein equation, and a “conventional complete gauge-fixing approach”, in which we use the spherical harmonic functions

Y_{l m}

as the scalar harmonics

S_{δ}

from the starting point. As the result of this comparison, we conclude that our gauge-invariant formulation and the above “conventional complete gauge-fixing approach” are different, though these two formulations lead similar solutions for

l = 0, 1

-mode perturbations. More specifically, there is a case where the boundary conditions and initial conditions are restricted in a “conventional complete gauge-fixing approach” where we use the decomposition of the metric perturbation by the spherical harmonics

Y_{l m}

from the starting point.

The organization of this paper is as follows. In Sec. 2, we briefly review the premise of our series of papers [12,13,14,15,16], which are necessary for the ingredients of this paper. We also emphasize the difference between the concepts of the first- and the second-kind gauges and summarize the linearized Einstein equations for

l = 0, 1

modes and their formal solutions in Sec. 2. In Sec. 3, we specify the rule of our comparison between our gauge-invariant formulation and a conventional gauge-fixing approach and summarize the gauge transformation rules for the metric perturbations of

l = 0, 1

modes, because the above statement “gauge-invariant formulations in general-relativistic perturbations are equivalent to complete gauge-fixing approaches” includes some ambiguous. In Sec. 4, we discuss the linearized Einstein equations for

l = 1

odd-modes and their solutions in the conventional gauge-fixing approach. In Sec. 5, we discuss the linearized Einstein equations for

l = 1

even-modes and their solutions in the conventional gauge-fixing approach. In Sec. 6, we derive the solution to the linearized Einstein equations for

l = 0

modes through the complete gauge-fixing and discuss the comparison with linearized LTB solution. Sec. 7 is devoted to the summary of this paper and discussions based on our results.

We use the notation used in the previous papers [12,13,14,15,16] and the unit

G = c = 1

, where G is Newton’s constant of gravitation and c is the velocity of light.

2. Brief Review of a Gauge-Invariant Treatment of $l = 0, 1$ Modes

In this section, we briefly review the premises of our series of papers [12,13,14,15,16] which are necessary for the ingredients of this paper. In Sec. 2.1, we review our framework of the gauge-invariant perturbation theory [34,35]. This is an important premise of the series of our papers [12,13,14,15,16] and this paper. In Sec. 2.2, we review the gauge-invariant perturbation theory on spherically symmetric spacetimes which includes our proposal in Refs. [12,13,14,15,16]. In Sec. 2.3, we summarize the

l = 1

odd-mode linearized Einstein equations and their “formal” solutions. In Sec. 2.4, we summarize the

l = 0, 1

even-mode linearized Einstein equations and their “formal” solutions. The equations and their solutions in Sec. 2.3 and Sec. 2.4 are derived based on our proposal in Refs. [12,13,14,15,16]. These are necessary for the arguments within this paper.

2.1. General Framework of Gauge-Invariant Perturbation Theory

In any perturbation theory, we always treat two spacetime manifolds. One is the physical spacetime

(M_{ph}, {\bar{g}}_{a b})

, which is identified with our nature itself, and we want to describe this spacetime

(M_{ph}, {\bar{g}}_{a b})

by perturbations. The other is the background spacetime

(M, g_{a b})

, which is prepared as a reference by hand. Note that these two spacetimes are distinct. Furthermore, in any perturbation theory, we always write equations for the perturbation of the variable Q as follows:

Q (“ p ”) = Q_{0} (p) + δ Q (p) .

(1)

Equation (1) gives a relation between variables on different manifolds. Actually,

Q (“ p ”)

in Equation (1) is a variable on the physical spacetime

M_{ϵ} = M_{ph}

, whereas

Q_{0} (p)

and

δ Q (p)

are variables on the background spacetime

M

. Because we regard Equation (1) as a field equation, Equation (1) includes an implicit assumption of the existence of a point identification map

X_{ϵ}

M \to M_{ϵ}

p \in M \mapsto “ p ” \in M_{ϵ}

. This identification map is a gauge choice in general-relativistic perturbation theories. This is the notion of the second-kind gauge pointed out by Sachs [51,52,53,54]. Note that this second-kind gauge is a different notion from the degree of freedom of the coordinate transformation on a single manifold, which is called the first-kind gauge [14,40,41]. This distinction between the first- and the second-kind of gauges extensively explained in the Part I paper [14] and is also important to understand the ingredients of this paper.

To compare the variable Q on

M_{ϵ}

with its background value

Q_{0}

M

, we use the pull-back

X_{ϵ}^{*}

of the identification map

X_{ϵ}

M \to M_{ϵ}

and we evaluate the pulled-back variable

X_{ϵ}^{*} Q

on the background spacetime

M

. Furthermore, in perturbation theories, we expand the pull-back operation

X_{ϵ}^{*}

to the variable Q with respect to the infinitesimal parameter

ϵ

for the perturbation as

\begin{matrix} X_{ϵ}^{*} Q = Q_{0} + ϵ {}_{X}^{(1)}Q + O (ϵ^{2}) . \end{matrix}

(2)

Equation (2) are evaluated on the background spacetime

M

. When we have two different gauge choices

X_{ϵ}

and

Y_{ϵ}

, we can consider the gauge transformation, which is the change of the point-identification

X_{ϵ} \to Y_{ϵ}

. This gauge transformation is given by the diffeomorphism

Φ_{ϵ}

: =

{(X_{ϵ})}^{- 1} \circ Y_{ϵ}

M

→

M

. Actually, the diffeomorphism

Φ_{ϵ}

induces a pull-back from the representation

X_{ϵ}^{*} Q_{ϵ}

to the representation

Y_{ϵ}^{*} Q_{ϵ}

Y_{ϵ}^{*} Q_{ϵ} (q) = Φ_{ϵ}^{*} X_{ϵ}^{*} Q_{ϵ} (q)

at any point

q \in M

. From general arguments of the Taylor expansion [55,56,57], the pull-back

Φ_{ϵ}^{*}

is expanded as

\begin{matrix} Y_{ϵ}^{*} Q_{ϵ} (q) & = & X_{ϵ}^{*} Q_{ϵ} (q) + ϵ £_{ξ_{(1)}} X_{ϵ}^{*} Q_{ϵ} (q) + O (ϵ^{2}), \end{matrix}

(3)

where

ξ_{(1)}^{a}

is the generator of

Φ_{ϵ}

. From Equations (2) and (3), the gauge transformation for the first-order perturbation

{}^{(1)}Q

is given by

\begin{matrix} {}_{Y}^{(1)} Q (q) - {}_{X}^{(1)} Q (q) & = & £_{ξ_{(1)}} Q_{0} (q) \end{matrix}

(4)

at any point

q \in M

. We also employ the order by order gauge invariance as a concept of gauge invariance [34,35]. We call the kth-order perturbation

{}_{X}^{(k)} Q

as gauge invariant if and only if

\begin{matrix} {}_{X}^{(k)} Q (q) = {}_{Y}^{(k)} Q (q) \end{matrix}

(5)

for any gauge choice

X_{ϵ}

and

Y_{ϵ}

at any point of

q \in M

Based on the above setup, we proposed a formulation to construct gauge-invariant variables of higher-order perturbations [34,35]. First, we expand the metric on the physical spacetime

M_{ϵ}

, which was pulled back to the background spacetime

M

through a gauge choice

X_{ϵ}

\begin{matrix} X_{ϵ}^{*} {\bar{g}}_{a b} & = & g_{a b} + ϵ {}_{X} h_{a b} + O (ϵ^{2}) . \end{matrix}

(6)

Although the expression (6) depends entirely on the gauge choice

X_{ϵ}

, henceforth, we do not explicitly express the index of the gauge choice

X_{ϵ}

in the expression if there is no possibility of confusion. The important premise of our formulation of higher-order gauge-invariant perturbation theory was the following conjecture [34,35] for the linear metric perturbation

h_{a b}

Conjecture 2.1.

If the gauge transformation rule for a perturbative pulled-back tensor field

h_{a b}

from the physical spacetime

M_{ϵ}

to the background spacetime

M

is given by

{}_{Y} h_{a b}

−

{}_{X} h_{a b}

£_{ξ_{(1)}} g_{a b}

with the background metric

g_{a b}

, there then exist a tensor field

F_{a b}

and a vector field

Y^{a}

such that

h_{a b}

is decomposed as

h_{a b}

= :

F_{a b}

£_{Y} g_{a b}

, where

F_{a b}

and

Y^{a}

are transformed as

{}_{Y} F_{a b}

−

{}_{X} F_{a b}

= 0 and

{}_{Y} Y^{a}

−

{}_{X} Y^{a}

ξ_{(1)}^{a}

under the gauge transformation, respectively.

We call

F_{a b}

and

Y^{a}

as the gauge-invariant and gauge-dependent parts of

h_{a b}

, respectively.

The proof of Conjecture 2.1 is highly nontrivial [36,37,38], and it was found that the gauge-invariant variables are essentially non-local. Despite this non-triviality, once we accept Conjecture 2.1, we can decompose the linear perturbation of an arbitrary tensor field

{}_{X}^{(1)} Q

, whose gauge transformation is given by Equation (4), through the gauge-dependent part

Y_{a}

of the metric perturbation in Conjecture 2.1 as

\begin{matrix} {}_{X}^{(1)} Q = {}^{(1)} Q + £_{{}_{X} Y} Q_{0}, \end{matrix}

(7)

where

{}^{(1)} Q

is the gauge-invariant part of the perturbation

{}_{X}^{(1)} Q

. As examples, the linearized Einstein tensor

{}_{X}^{(1)}G_{a}^{b}

and the linear perturbation of the energy-momentum tensor

{}_{X}^{(1)}T_{a}^{b}

are also decomposed as

\begin{matrix} {}_{X}^{(1)} G_{a}^{b} = {}^{(1)} G_{a}^{b} [F] + £_{{}_{X} Y} G_{a}^{b}, {}_{X}^{(1)} T_{a}^{b} = {}^{(1)} T_{a}^{b} + £_{{}_{X} Y} T_{a}^{b}, \end{matrix}

(8)

where

G_{a b}

and

T_{a b}

are the background values of the Einstein tensor and the energy-momentum tensor, respectively [35,46]. Using the background Einstein equation

G_{a}^{b} = 8 π T_{a}^{b}

, the linearized Einstein equation

{}_{X}^{(1)} G_{a b} = 8 π {}_{X}^{(1)} T_{a b}

is automatically given in the gauge-invariant form

\begin{matrix} {}^{(1)} G_{a}^{b} [F] = 8 π {}^{(1)} T_{a}^{b} [F, ϕ] \end{matrix}

(9)

even if the background Einstein equation is nontrivial. Here, “

ϕ

” in Equation (9) symbolically represents the matter degree of freedom.

Finally, we comment on the coordinate transformation induced by the gauge transformation

Φ_{ϵ}

of the second-kind [12,40]. To see this, we introduce the coordinate system

{O_{α}, ψ_{α}}

on the background spacetime

M

, where

O_{α}

are open sets on the background spacetime and

ψ_{α}

are diffeomorphisms from

O_{α}

R^{4}

(

4 = dim M

). The coordinate system

{O_{α}, ψ_{α}}

is the set of collections of the pair of open sets

O_{α}

and diffeomorphism

ψ_{α} : O_{α} \mapsto R^{4}

. If we employ a gauge choice

X_{ϵ}

of the second kind, we have the correspondence of the physical spacetime

M_{ϵ}

and the background spacetime

M

. Together with the coordinate system

ψ_{α}

M

, this correspondence

X_{ϵ}

between

M_{ϵ}

and

M

induces the coordinate system on

M_{ϵ}

. Actually,

X_{ϵ} (O_{α})

for each

α

is an open set of

M_{ϵ}

. Then,

ψ_{α} \circ X_{ϵ}^{- 1}

becomes a diffeomorphism from an open set

X_{ϵ} (O_{α}) \subset M_{ϵ}

R^{4}

. This diffeomorphism

ψ_{α} \circ X_{ϵ}^{- 1}

induces a coordinate system of an open set on

M_{ϵ}

. When we have two different gauge choices

X_{ϵ}

and

Y_{ϵ}

of the second kind,

ψ_{α} \circ X_{ϵ}^{- 1}

M_{ϵ}

↦

R^{4}

(

{x^{μ}}

) and

ψ_{α} \circ Y_{ϵ}^{- 1}

M_{ϵ}

↦

R^{4}

(

{y^{μ}}

) become different coordinate systems on

M_{ϵ}

. We can also consider the coordinate transformation from the coordinate system

ψ_{α} \circ X_{ϵ}^{- 1}

to another coordinate system

ψ_{α} \circ Y_{ϵ}^{- 1}

. Because the gauge transformation

X_{ϵ} \to Y_{ϵ}

is induced by the diffeomorphism

Φ_{ϵ}

: =

{(X_{ϵ})}^{- 1} \circ Y_{ϵ}

, this diffeomorphism

Φ_{ϵ}

induces the coordinate transformation as

\begin{matrix} y^{μ} (q) : = x^{μ} (p) = ({(Φ_{ϵ}^{- 1})}^{*} x^{μ}) (q) \end{matrix}

(10)

in the passive point of view [34,55], where p, q∈

M

are identified to the same point

` ` p "

∈

M_{ϵ}

by the gauge choices

X_{ϵ}

and

Y_{ϵ}

, respectively. If we represent this coordinate transformation in terms of the Taylor expansion (3), we have the coordinate transformation

\begin{matrix} y^{μ} (q) = x^{μ} (q) - ϵ ξ_{(1)}^{μ} (q) + O (ϵ^{2}) . \end{matrix}

(11)

We should emphasize that the coordinate transformation (11) is not the starting point of the gauge transformation but a result of the above framework.

On the other hand, we may consider the point replacement by the one-parameter diffeomorphism

s = Ψ_{λ} (r)

, where

s, r \in M_{ϵ}

and

λ

is an infinitesimal parameter satisfying

Ψ_{λ = 0} (r) = r

. The pull-back

Ψ_{λ}^{*}

of any tensor field Q on

M_{ϵ}

is given by

\begin{matrix} Q (s) & = & Q (Ψ_{λ} (r)) = (Ψ_{λ}^{*}) Q (r) \\ = & Q (r) + λ {£_{ζ} Q|}_{λ = 0} (r) + O (λ^{2}), \end{matrix}

(12)

where

ζ^{a}

is the generator of the pull-back

Ψ_{λ}^{*}

. Equation (12) is just the formula of the Taylor expansion on the manifold

M_{ϵ}

without using any coordinate system. At the same time, Equation (12) is the definitions of the Lie derivative

£_{ζ}

and its generator

ζ^{a}

. In many literatures, this formula is derived from the coordinate transformation

\begin{matrix} y^{μ} (s) : = x^{μ} (r) + λ ζ^{μ} (r) + O (λ^{2}) \end{matrix}

(13)

as explained in the Part I paper [14]. The formula (12) of the Taylor expansion defined without any coordinate system and the second term in the right-hand side of Equation (12) represents the actual difference of the tensor fields

Q (s)

and

Q (r)

in the different point

s \neq r

and its physical meaning.

If we consider a formal metric decomposition

{\bar{g}}_{a b} = {}^{(0)} g_{a b} + λ h_{a b} + O (λ^{2})

within

M_{ϵ}

as an example of the tensor field Q in Equation (12), the formula (12) is given by

\begin{matrix} {}^{(0)}g_{a b} (s) + λ h_{a b} (s) = {}^{(0)}g_{a b} (r) + λ (h_{a b} (r) + {£_{ζ} {}^{(0)}g_{a b}|}_{r}) + O (λ^{2}) . \end{matrix}

(14)

Since the formula of the Taylor expansion (12) is derived from the infinitesimal coordinate transformation rule (13) in many literatures, the term

{£_{ζ} {}^{(0)}g_{a b}|}_{r}

in the right-hand side of Equation (14) is often called “the degree of freedom of the coordinate transformation” and “unphysical degree of freedom”. However, since the formula (14) is just the re-expression of the Taylor expansion (12) defined without any coordinate system and the term

{£_{ζ} {}^{(0)}g_{a b}|}_{r}

in Equation (14) should have its physical meaning. If we insist that the term

{£_{ζ} {}^{(0)}g_{a b}|}_{r}

which appears due to the point replacement on the single manifold is “unphysical”, this directly leads the statement that “the famous arguments of the Killing vector and the symmetry of the spacetime are physically meaningless.” For this reason, we have to emphasize that we cannot regard the second term of the right-hand side of Equation (12) as an “unphysical degree of freedom.”

In our series of papers [12,13,14,15,16] and in this paper, we classify the term

{£_{ζ} {}^{(0)}g_{a b}|}_{r}

in Equation (14) as one of gauge-degree of freedom of the first kind, since this term can be eliminate the infinitesimal coordinate transformation (13) which is the coordinate transformation within the single manifold

M_{ϵ}

. Furthermore, Equation (14) does not mean

h_{a b} (s)

h_{a b} (r)

{£_{ζ} {}^{(0)}g_{a b}|}_{r}

but it just means

{}^{(0)}g_{a b} (s)

{}^{(0)}g_{a b} (r)

λ {£_{ζ} {}^{(0)}g_{a b}|}_{r}

O (λ^{2})

. Moreover, we also have to emphasize that the infinitesimal coordinate transformation (13) is essentially different from the infinitesimal coordinate transformation (11). Actually, the infinitesimal coordinate transformation (13) is the replacement of the point within the single manifold

M_{ϵ}

. On the other hand, the coordinate transformation (11) is just the change of the coordinate label at the same point in the background spacetime

M

2.2. Linear perturbations on spherically symmetric background spacetime

Here, we consider the 2+2 formulation of the perturbation of a spherically symmetric background spacetime, which originally proposed by Gerlach and Sengupta [25,26,27,28]. Spherically symmetric spacetimes are characterized by the direct product

M = M_{1} \times S^{2}

and their metric is

\begin{matrix} g_{a b} & = & y_{a b} + r^{2} γ_{a b}, \end{matrix}

(15)

\begin{matrix} y_{a b} & = & y_{A B} {(d x^{A})}_{a} {(d x^{B})}_{b}, γ_{a b} = γ_{p q} {(d x^{p})}_{a} {(d x^{q})}_{b}, \end{matrix}

(16)

where

x^{A} = (t, r)

x^{p} = (θ, ϕ)

, and

γ_{p q}

is the metric on the unit sphere. In the Schwarzschild spacetime, the metric (15) is given by

\begin{matrix} y_{a b} & = & - f {(d t)}_{a} {(d t)}_{b} + f^{- 1} {(d r)}_{a} {(d r)}_{b}, f = 1 - \frac{2 M}{r}, \end{matrix}

(17)

\begin{matrix} γ_{a b} & = & {(d θ)}_{a} {(d θ)}_{b} + {sin}^{2} θ {(d ϕ)}_{a} {(d ϕ)}_{b} = θ_{a} θ_{b} + ϕ_{a} ϕ_{b}, \end{matrix}

(18)

\begin{matrix} θ_{a} & = & {(d θ)}_{a}, ϕ_{a} = sin θ {(d ϕ)}_{a} . \end{matrix}

(19)

On this background spacetime

(M, g_{a b})

, the components of the metric perturbation is given by

\begin{matrix} h_{a b} = h_{A B} {(d x^{A})}_{a} {(d x^{B})}_{b} + 2 h_{A p} {(d x^{A})}_{(a} {(d x^{p})}_{b)} + h_{p q} {(d x^{p})}_{a} {(d x^{q})}_{b} . \end{matrix}

(20)

Here, we note that the components

h_{A B}

h_{A p}

, and

h_{p q}

are regarded as components of scalar, vector, and tensor on

S^{2}

, respectively. In the Part I paper [14], we showed the linear independence of the set of harmonic functions

\begin{matrix} \{S_{δ}, {\hat{D}}_{p} S_{δ}, ϵ_{p q} {\hat{D}}^{q} S_{δ}, \frac{1}{2} γ_{p q} S_{δ}, ({\hat{D}}_{p} {\hat{D}}_{q} - \frac{1}{2} γ_{p q}) S_{δ}, 2 ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} S_{δ}\}, \end{matrix}

(21)

where

{\hat{D}}_{p}

is the covariant derivative associated with the metric

γ_{p q}

S^{2}

{\hat{D}}^{p} = γ^{p q} {\hat{D}}_{q}

ϵ_{p q} = ϵ_{[p q]} = 2 θ_{[p} ϕ_{q]}

is the totally antisymmetric tensor on

S^{2}

. In the set of harmonic function (21), the scalar harmonic function

S_{δ}

is given by

\begin{matrix} S_{δ} = \{\begin{matrix} Y_{l m} & f o r & l \geq 2; \\ k_{(\hat{Δ} + 2) m} & f o r & l = 1; \\ k_{(\hat{Δ})} & f o r & l = 0 . \end{matrix} \end{matrix}

(22)

Here, functions

k_{(\hat{Δ})}

and

k_{(\hat{Δ} + 2) m}

are the kernel modes of the derivative operator

\hat{Δ}

and

[\hat{Δ} + 2]

, respectively, and we employ the explicit form of these functions as

\begin{matrix} k_{(\hat{Δ})} & = & 1 + δ ln {(\frac{1 - cos θ}{1 + cos θ})}^{1 / 2}, δ \in R, \end{matrix}

(23)

\begin{matrix} k_{(\hat{Δ} + 2, m = 0)} & = & cos θ + δ (\frac{1}{2} cos θ ln \frac{1 + cos θ}{1 - cos θ} - 1), δ \in R, \end{matrix}

(24)

\begin{matrix} k_{(\hat{Δ} + 2, m = \pm 1)} & = & [sin θ + δ (+ \frac{1}{2} sin θ ln \frac{1 + cos θ}{1 - cos θ} + cot θ)] e^{\pm i ϕ} . \end{matrix}

(25)

Then, we consider the mode decomposition of the components

{h_{A B}, h_{A p}, h_{p q}}

as follows:

\begin{matrix} h_{A B} & = & \sum_{l, m} {\tilde{h}}_{A B} S_{δ}, \end{matrix}

(26)

\begin{matrix} h_{A p} & = & r \sum_{l, m} [{\tilde{h}}_{(e 1) A} {\hat{D}}_{p} S_{δ} + {\tilde{h}}_{(o 1) A} ϵ_{p q} {\hat{D}}^{q} S_{δ}], \end{matrix}

(27)

\begin{matrix} h_{p q} & = & r^{2} \sum_{l, m} [\frac{1}{2} γ_{p q} {\tilde{h}}_{(e 0)} S_{δ} + {\tilde{h}}_{(e 2)} ({\hat{D}}_{p} {\hat{D}}_{q} - \frac{1}{2} γ_{p q} {\hat{D}}^{r} {\hat{D}}_{r}) S_{δ} + 2 {\tilde{h}}_{(o 2)} ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} S_{δ}] . \end{matrix}

(28)

Since the linear independence of each element of the set of harmonic function (21) is guaranteed, the one-to-one correspondence between the components

{h_{A B},

h_{A p},

h_{p q}}

and the mode coefficients

{{\tilde{h}}_{A B},

{\tilde{h}}_{(e 1) A},

{\tilde{h}}_{(o 1) A},

{\tilde{h}}_{(e 0)},

{\tilde{h}}_{(e 2)},

{\tilde{h}}_{(o 2)}}

with the decomposition formulae (26)-(28) is guaranteed including

l = 0, 1

mode if

δ \neq 0

. Then, the mode-by-mode analysis including

l = 0, 1

is possible when

δ \neq 0

. However, the mode functions (23)–(25) are singular if

δ \neq 0

. When

δ = 0

, we have

k_{(\hat{Δ})} \propto Y_{00}

and

k_{(\hat{Δ} + 2) m} \propto Y_{1 m}

, but the linear dependence of the set of harmonics (21) is lost in this case. Because of this situation, we proposed the following strategy:

Proposal 2.1.

We decompose the metric perturbation

h_{a b}

on the background spacetime with the metric (15)–(18) through Equations (26)–(28) with the harmonic function

S_{δ}

given by Equation (22). Then, Equations (26)–(28) become invertible including

l = 0, 1

modes. After deriving the mode-by-mode field equations such as linearized Einstein equations by using the harmonic functions

S_{δ}

, we choose

δ = 0

as the regular boundary condition for solutions when we solve these field equations.

As shown in the Part I paper [14], once we accept Proposal 2.1, the Conjecture 2.1 becomes the following statement:

Theorem 1.

If the gauge-transformation rule for a perturbative pulled-back tensor field

h_{a b}

to the background spacetime

M

is given by

{}_{Y} h_{a b}

−

{}_{X} h_{a b}

£_{ξ_{(1)}} g_{a b}

with the background metric

g_{a b}

with spherically symmetry, there then exist a tensor field

F_{a b}

and a vector field

Y^{a}

such that

h_{a b}

is decomposed as

h_{a b}

= :

F_{a b}

£_{Y} g_{a b}

, where

F_{a b}

and

Y^{a}

are transformed into

{}_{Y} F_{a b}

−

{}_{X} F_{a b}

= 0 and

{}_{Y} Y^{a}

−

{}_{X} Y^{a}

ξ_{(1)}^{a}

under the gauge transformation, respectively.

Actually, the gauge-dependent variable

Y_{a}

is given by

\begin{matrix} Y_{a} & : = & \sum_{l, m} {\tilde{Y}}_{A} S_{δ} {(d x^{A})}_{a} + \sum_{l, m} ({\tilde{Y}}_{(e 1)} {\hat{D}}_{p} S_{δ} + {\tilde{Y}}_{(o 1)} ϵ_{p q} {\hat{D}}^{q} S_{δ}) {(d x^{p})}_{a}, \end{matrix}

(29)

where

\begin{matrix} {\tilde{Y}}_{A} & : = & r {\tilde{h}}_{(e 1) A} - \frac{r^{2}}{2} {\bar{D}}_{A} {\tilde{h}}_{(e 2)}, \end{matrix}

(30)

\begin{matrix} {\tilde{Y}}_{(e 1)} & : = & \frac{r^{2}}{2} {\tilde{h}}_{(e 2)}, \end{matrix}

(31)

\begin{matrix} {\tilde{Y}}_{(o 1)} & : = & - r^{2} {\tilde{h}}_{(o 2)} . \end{matrix}

(32)

Furthermore, including

l = 0, 1

modes, the components of the gauge-invariant part

F_{a b}

of the metric perturbation

h_{a b}

is given by

\begin{matrix} F_{A B} & = & \sum_{l, m} {\tilde{F}}_{A B} S_{δ}, \end{matrix}

(33)

\begin{matrix} F_{A p} & = & r \sum_{l, m} {\tilde{F}}_{A} ϵ_{p q} {\hat{D}}^{q} S_{δ}, {\hat{D}}^{p} F_{A p} = 0, \end{matrix}

(34)

\begin{matrix} F_{p q} & = & \frac{1}{2} γ_{p q} r^{2} \sum_{l, m} \tilde{F} S_{δ}, \end{matrix}

(35)

where

{\tilde{F}}_{A B}

{\tilde{F}}_{A}

, and

\tilde{F}

are given by

\begin{matrix} {\tilde{F}}_{A B} & : = & {\tilde{h}}_{A B} - 2 {\bar{D}}_{(A} {\tilde{Y}}_{B)}, \end{matrix}

(36)

\begin{matrix} {\tilde{F}}_{A} & : = & {\tilde{h}}_{(o 1) A} + r {\bar{D}}_{A} {\tilde{h}}_{(o 2)}, \end{matrix}

(37)

\begin{matrix} \tilde{F} & : = & {\tilde{h}}_{(e 0)} - \frac{4}{r} {\tilde{Y}}_{A} {\bar{D}}^{A} r + {\tilde{h}}_{(e 2)} l (l + 1) . \end{matrix}

(38)

Thus, we have constructed gauge-invariant metric perturbations on the Schwarzschild background spacetime including

l = 0, 1

modes.

Furthermore, from Equations (33)–() for the gauge-invariant variables

F_{A B}

F_{A p}

, and

F_{p q}

and gauge-dependent variables

Y_{a}

defined by Equations (29)–(), the original components

{h_{A B}, h_{A p}, h_{p q}}

of the metric perturbation (26)–() are given by

\begin{matrix} h_{a b} & = & F_{a b} + £_{Y} g_{a b} . \end{matrix}

(39)

This is the assertion of Theorem 1.

The aim of our proposal is to add a greater degree of freedom of the metric perturbation so that the decomposition (39) is guaranteed even in the case of

l = 0, 1

modes. Therefore, it is impossible to reach the final expression (39) if we treat the metric perturbation by using

S_{δ = 0} = Y_{l m}

in the decomposition formulae (26)–(28) from the starting point.

To see this more specifically, we show an explicit example of the

l = 1

odd mode perturbation. If we apply our proposal to the decomposition formulae (26)–(28),

l = 1

odd-mode perturbation is given by

\begin{matrix} h_{a b} = 2 r {\tilde{h}}_{(o 1) A}^{(l = 1)} ϵ_{p q} {\hat{D}}^{q} S_{δ} {(d x^{A})}_{(a} {(d x^{p})}_{b)} + 2 r^{2} {\tilde{h}}_{(o 2)}^{(l = 1)} ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} S_{δ} {(d x^{p})}_{(a} {(d x^{q})}_{b)} . \end{matrix}

(40)

If we use

S_{δ = 0} = Y_{l m}

from the starting point,

2 ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} S_{δ} = 0

. So, the mode coefficient

{\tilde{h}}_{(o 2)}^{(l = 1)}

does not appear. When

δ \neq 0

, the gauge-transformation rule of the variables

{\tilde{h}}_{(o 1) A}^{(l = 1)}

and

{\tilde{h}}_{(o 2)}^{(l = 1)}

are given by

\begin{matrix} {}_{Y} {\tilde{h}}_{(o 1) A}^{(l = 1)} - {}_{X} {\tilde{h}}_{(o 1) A}^{(l = 1)} = r {\bar{D}}_{A} (\frac{1}{r} ζ_{(o)}), {}_{Y} {\tilde{h}}_{(o 2)}^{(l = 1)} - {}_{X} {\tilde{h}}_{(o 2)}^{(l = 1)} = - \frac{1}{r} ζ_{(o)}, \end{matrix}

(41)

where the generator of the gauge transformation is given by

ξ_{A} = 0

and

ξ_{p} = r ζ_{(o)} ϵ_{p q} {\hat{D}}^{q} S_{δ}

. If we use

S_{δ = 0} = Y_{l m}

from the starting point, the gauge-transformation rule for the variable

{\tilde{h}}_{(o 2)}^{(l = 1)}

does not appear, either. However, in our case, this gauge transformation appears due to the fact

ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} S_{δ} \neq 0

. Inspecting these gauge-transformation rules, we rewrite Equation (40) as

\begin{matrix} h_{a b} & = & 2 r [({\tilde{h}}_{(o 1) A}^{(l = 1)} + r {\bar{D}}_{A} {\tilde{h}}_{(o 2)}) - r {\bar{D}}_{A} {\tilde{h}}_{(o 2)}] ϵ_{p q} {\hat{D}}^{q} S_{δ} {(d x^{A})}_{(a} {(d x^{p})}_{b)} \\ + 2 r^{2} {\tilde{h}}_{(o 2)}^{(l = 1)} ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} S_{δ} {(d x^{p})}_{(a} {(d x^{q})}_{b)} \\ = & 2 r [{\tilde{F}}_{A} - r {\bar{D}}_{A} (\frac{1}{r^{2}} {\tilde{Y}}_{(o 1)})] ϵ_{p q} {\hat{D}}^{q} S_{δ} {(d x^{A})}_{(a} {(d x^{p})}_{b)} \\ + 2 r^{2} (\frac{1}{r^{2}} {\tilde{Y}}_{(o 1)}) ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} S_{δ} {(d x^{p})}_{(a} {(d x^{q})}_{b)} . \end{matrix}

(42)

In Equation (42),

{\tilde{F}}_{A}

is the gauge-invariant variable for the metric perturbation defined by Equation (37) and

{\tilde{Y}}_{(o 1)}

is the gauge-dependent part of the metric perturbation defined by Equation (32). The terms of

{\tilde{Y}}_{(o 1)}

in Equation (42) can be written in the form of the Lie derivative of the background metric as in Equation (39). When

δ = 0

, Equation (42) is given by

\begin{matrix} h_{a b} & = & 2 r [{\tilde{F}}_{A} - r {\bar{D}}_{A} (\frac{1}{r^{2}} {\tilde{Y}}_{(o 1)})] ϵ_{p q} {\hat{D}}^{q} S_{δ} {(d x^{A})}_{(a} {(d x^{p})}_{b)} . \end{matrix}

(43)

This is also given in the form (39).

When we construct the gauge-invariant variable

{\tilde{F}}_{A}

in Equations (42) and (43), the existence of the coefficient

{\tilde{h}}_{(o 2)}^{(l = 1)} = {\tilde{Y}}_{(o 1)} / r^{2}

is essential which does not appear in the treatment using the spherical harmonics

Y_{l m}

from the starting point. Actually, we cannot define the gauge-invariant variable for

l = 1

odd-mode perturbation in the same manner as

l \geq 2

-mode case. Our proposal 2.1, make the degree of freedom of the metric perturbations increase. We have to emphasize that we can reach the decomposition (39) owing to this additional degree of freedom.

To discuss the linearized Einstein equation (9) and the linear perturbation of the continuity equation

\begin{matrix} \nabla_{a} {}^{(1)} T_{b}^{a} = 0 \end{matrix}

(44)

of the gauge-invariant energy-momentum tensor

{}^{(1)} T_{b}^{a} : = g^{a c} {}^{(1)} T_{b c}

on a vacuum background spacetime, we consider the mode-decomposition of the gauge-invariant part

{}^{(1)} T_{b c}

of the linear perturbation of the energy-momentum tensor through the set (21) of the harmonics as follows:

\begin{matrix} {}^{(1)} T_{a b} & = & \sum_{l, m} {\tilde{T}}_{A B} S_{δ} {(d x^{A})}_{a} {(d x^{B})}_{b} + r \sum_{l, m} \{{\tilde{T}}_{(e 1) A} {\hat{D}}_{p} S_{δ} + {\tilde{T}}_{(o 1) A} ϵ_{p r} {\hat{D}}^{r} S_{δ}\} 2 {(d x^{A})}_{(a} {(d x^{p})}_{b)} \\ + r^{2} \sum_{l, m} \{{\tilde{T}}_{(e 0)} \frac{1}{2} γ_{p q} S_{δ} + {\tilde{T}}_{(e 2)} ({\hat{D}}_{p} {\hat{D}}_{q} S_{δ} - \frac{1}{2} γ_{p q} {\hat{D}}_{r} {\hat{D}}^{r} S_{δ}) \\ + {\tilde{T}}_{(o 2)} 2 ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} S_{δ}\} {(d x^{p})}_{a} {(d x^{q})}_{b} . \end{matrix}

(45)

In the Part I paper [14], we derived the linearized Einstein equations, discussed the odd-mode perturbation

{\tilde{F}}_{A p}

in Equation (34), and derived the

l = 1

odd-mode solutions to these equations. The Einstein equation for even mode

{\tilde{F}}_{A B}

and

\tilde{F}

in Equations (33) and (35) also derived in the Part I paper [14], and

l = 0, 1

even-mode solutions are derived in the Part II paper [15]. Since these solutions include the Kerr parameter perturbation and the Schwarzschild mass parameter perturbation of the linear order in the vacuum case, these are physically reasonable. Then, we conclude that our proposal is also physically reasonable. Furthermore, we also checked that our derived solutions include the linearized LTB solution and non-rotating C-metric with the Schwarzschild background in the Part III paper [16].

The purpose of this paper is to compare our proposed gauge-invariant treatments for

l = 0, 1

-mode perturbations on the Schwarzschild background spacetime with conventional “complete gauge-fixing treatments” in which we use the spherical harmonics

Y_{l m}

from the starting point. For this purpose, the linearized Einstein equations for the

l = 0, 1

-modes and their solutions based on our proposal are necessary. Therefore, we review them below.

2.3. $l = 1$ Odd-Mode Linearized Einstein Equations and Solutions

As derived in the Part I paper [14], the

l = 1

odd-mode part in the linearized Einstein equations are simplified as the constraint equation

\begin{matrix} {\bar{D}}_{D} (r {\tilde{F}}^{D}) = 0, \end{matrix}

(46)

and the evolution equation

\begin{matrix} - [{\bar{D}}^{D} {\bar{D}}_{D} - \frac{2}{r^{2}}] (r {\tilde{F}}_{A}) - \frac{2}{r^{2}} ({\bar{D}}^{D} r) ({\bar{D}}_{A} r) (r {\tilde{F}}_{D}) + \frac{2}{r} ({\bar{D}}^{D} r) {\bar{D}}_{A} (r {\tilde{F}}_{D}) \\ = & 16 π r {\tilde{T}}_{(o 1) A}, \end{matrix}

(47)

where we choose

{\tilde{T}}_{(o 2)} = 0

by hand. Furthermore, we have the continuity equation

\begin{matrix} {\bar{D}}^{C} {\tilde{T}}_{(o 1) C} + \frac{3}{r} ({\bar{D}}^{D} r) {\tilde{T}}_{(o 1) D} = 0 \end{matrix}

(48)

for the

l = 1

odd-mode matter perturbation which is derived from the divergence of the first-order perturbation of the energy-momentum tensor.

We also note that the constraint (46) comes from the traceless part of the

(q, p)

-component of the Einstein equation (9), which is the coefficient of the mode function

2 ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{p} S_{δ}

. If

δ = 0

, i.e., the scalar harmonics

S_{δ}

is the spherical harmonics

Y_{l m}

2 ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{p} S_{δ} = 0

for

l = 1

. Therefore, the constraint (46) does not appear when we use the spherical harmonics

Y_{l m}

from the starting point.

The explicit strategy to solve these odd-mode perturbations and

l = 0, 1

mode solutions was discussed in the Part I paper [14]. As the result, we obtained the

l = 1

odd-mode “formal” solution as follows:

\begin{matrix} 2 F_{A p} {(d x^{A})}_{(a} {(d x^{p})}_{b)} = 6 M r^{2} [\int d r \frac{a_{1} (t, r)}{r^{4}}] {sin}^{2} θ {(d t)}_{(a} {(d ϕ)}_{b)} + £_{V} g_{a b}, \end{matrix}

(49)

\begin{matrix} V_{a} = (β_{1} t + β_{0} + W_{(o)} (t, r)) r^{2} {sin}^{2} θ {(d ϕ)}_{a}, \end{matrix}

(50)

where

\begin{matrix} a_{1} (t, r) & = & - \frac{16 π}{3 M} r^{3} f \int d t {\tilde{T}}_{(o 1) r} + a_{10} \\ = & - \frac{16 π}{3 M} \int d r r^{3} \frac{1}{f} {\tilde{T}}_{(o 1) t} + a_{10} . \end{matrix}

(51)

The constant

a_{10}

in Equation (51) corresponds to the Kerr parameter. Furthermore, the function

W_{(o)} (t, r)

in Equation (50) is related to the solution to the

l = 1

-mode Regge-Wheeler equation

\begin{matrix} \partial_{t}^{2} Z_{(o)} - f \partial_{r} (f \partial_{r} Z_{(o)}) + \frac{1}{r^{2}} f [l (l + 1) - 3 (1 - f)] Z_{(o)} = 16 π f^{2} {\tilde{T}}_{(o 1) r}, \end{matrix}

(52)

where

Z_{(o)} = r f \partial_{r} W_{(o)}

. We have to solve Equation (52) to obtain the function

W_{(o)} (t, r)

. In this sense, the solution () should be regarded as the “formal” one.

2.4. $l = 0, 1$ even-mode linearized Einstein equations and solutions

The

l = 0, 1

even-mode part of the linearized Einstein equation (9) is summarized as follows:

\begin{matrix} {\tilde{F}}_{D}^{D} & = & 0, \end{matrix}

(53)

\begin{matrix} {\bar{D}}^{D} {\tilde{F}}_{A D} - \frac{1}{2} {\bar{D}}_{A} \tilde{F} & = & 16 π r {\tilde{T}}_{(e 1) A}, \end{matrix}

(54)

where the variable

{\tilde{F}}_{A B}

is the traceless part of the variable

{\tilde{F}}_{A B}

defined by

\begin{matrix} {\tilde{F}}_{A B} : = {\tilde{F}}_{A B} - \frac{1}{2} y_{A B} {\tilde{F}}_{C}^{C} \end{matrix}

(55)

and we choose the component of the energy-momentum tensor so that

{\tilde{T}}_{(e 2)} = 0

by hand. Owing to the same choice

{\tilde{T}}_{(e 2)} = 0

, we also have the evolution equations

\begin{matrix} ({\bar{D}}_{D} {\bar{D}}^{D} + \frac{2}{r} ({\bar{D}}^{D} r) {\bar{D}}_{D} - \frac{(l - 1) (l + 2)}{r^{2}}) \tilde{F} - \frac{4}{r^{2}} ({\bar{D}}_{C} r) ({\bar{D}}_{D} r) {\tilde{F}}^{C D} = 16 π S_{(F)}, \end{matrix}

(56)

\begin{matrix} S_{(F)} : = {\tilde{T}}_{C}^{C} + 4 ({\bar{D}}_{D} r) {\tilde{T}}_{(e 1)}^{D}, \\ [- {\bar{D}}_{D} {\bar{D}}^{D} - \frac{2}{r} ({\bar{D}}_{D} r) {\bar{D}}^{D} + \frac{4}{r} ({\bar{D}}^{D} {\bar{D}}_{D} r) + \frac{l (l + 1)}{r^{2}}] {\tilde{F}}_{A B} \\ + \frac{4}{r} ({\bar{D}}^{D} r) {\bar{D}}_{(A} {\tilde{F}}_{B) D} - \frac{2}{r} ({\bar{D}}_{(A} r) {\bar{D}}_{B)} \tilde{F} \end{matrix}

(57)

\begin{matrix} = 16 π S_{(F) A B}, \end{matrix}

(58)

\begin{matrix} S_{(F) A B} & : = & {\tilde{T}}_{A B} - \frac{1}{2} y_{A B} {\tilde{T}}_{C}^{C} - 2 ({\bar{D}}_{(A} (r {\tilde{T}}_{(e 1) B)}) - \frac{1}{2} y_{A B} {\bar{D}}^{D} (r {\tilde{T}}_{(e 1) D})) \\ + 2 y_{A B} ({\bar{D}}^{C} r) {\tilde{T}}_{(e 1) C}, \end{matrix}

(59)

for the variable

\tilde{F}

and the traceless variable

{\tilde{F}}_{A B}

with

l = 0, 1

. We also have to take into account the even-mode part of the continuity equation as follows:

\begin{matrix} {\bar{D}}^{C} {\tilde{T}}_{C}^{B} + \frac{2}{r} ({\bar{D}}^{D} r) {\tilde{T}}_{D}^{B} - \frac{1}{r} l (l + 1) {\tilde{T}}_{(e 1)}^{B} - \frac{1}{r} ({\bar{D}}^{B} r) {\tilde{T}}_{(e 0)} = 0, \end{matrix}

(60)

\begin{matrix} {\bar{D}}^{C} {\tilde{T}}_{(e 1) C} + \frac{3}{r} ({\bar{D}}^{C} r) {\tilde{T}}_{(e 1) C} + \frac{1}{2 r} {\tilde{T}}_{(e 0)} = 0, \end{matrix}

(61)

for

l = 0, 1

We also note that the constraint (53) comes from the traceless part of the

(q, p)

-component of the Einstein tensor (9), which is the coefficient of the mode function

({\hat{D}}_{p} {\hat{D}}_{q} - \frac{1}{2} γ_{p q} {\hat{D}}^{r} {\hat{D}}_{r}) S_{δ}

. If

δ = 0

, i.e., the scalar harmonics

S_{δ}

is the spherical harmonics

Y_{l m}

({\hat{D}}_{p} {\hat{D}}_{q} - \frac{1}{2} γ_{p q} {\hat{D}}^{r} {\hat{D}}_{r}) S_{δ} = 0

for

l = 1

. Therefore, the constraint (53) does not appear when we use the spherical harmonics

Y_{l m}

from the starting point.

2.4.1. $l = 1$ Even-Mode Solution

In the Part II paper [15], we derived the

l = 1

solution to Equations (53), (), (56), (), (60), and () with

l = 1

. For

m = 0

mode, in the Part II paper [15], we derived the following “formal” solution to the linearized Einstein equation

\begin{matrix} F_{a b} & = & £_{V} g_{a b} - \frac{16 π r^{2}}{3 (1 - f)} [f^{2} \{\frac{1 + f}{2} {\tilde{T}}_{r r} + r f \partial_{r} {\tilde{T}}_{r r} - {\tilde{T}}_{(e 0)} - 4 {\tilde{T}}_{(e 1) r}\} {(d t)}_{a} {(d t)}_{b} \\ + \frac{2 r}{f} \{\partial_{t} {\tilde{T}}_{t t} - \frac{3 f (1 - f)}{2 r} {\tilde{T}}_{t r}\} {(d t)}_{(a} {(d r)}_{b)} \\ + \frac{r}{f} \{\partial_{r} {\tilde{T}}_{t t} - \frac{3 (1 - 3 f)}{2 r f} {\tilde{T}}_{t t}\} {(d r)}_{a} {(d r)}_{b} \\ + r^{2} {\tilde{T}}_{t t} γ_{a b}] cos θ, \end{matrix}

(62)

where the vector field

V_{a}

is given by

\begin{matrix} V_{a} & : = & - r \partial_{t} Φ_{(e)} cos θ {(d t)}_{a} + (Φ_{(e)} - r \partial_{r} Φ_{(e)}) cos θ {(d r)}_{a} - r Φ_{(e)} sin θ {(d θ)}_{a} . \end{matrix}

(63)

Here, the variable

Φ_{(e)}

is a solution to the

l = 1

Zerilli equation

\begin{matrix} - \partial_{t}^{2} Φ_{(e)} + f \partial_{r} [f \partial_{r} Φ_{(e)}] - \frac{f (1 - f)}{r^{2}} Φ_{(e)} \\ = & \frac{4 π r}{3 (1 - f)} [3 (1 - 3 f) {\tilde{T}}_{t t} + (1 + f) f^{2} {\tilde{T}}_{r r} - 2 r f \partial_{r} {\tilde{T}}_{t t} \\ + 2 r f^{3} \partial_{r} {\tilde{T}}_{r r} - 2 f^{2} {\tilde{T}}_{(e 0)} - 8 f^{2} {\tilde{T}}_{(e 1) r}] . \end{matrix}

(64)

If we obtain the solution to the

l = 1

Zerilli equation (64), we can write the explicit form of the solution (62) through the generator

V_{a}

defined by Equation (63). In this sense, we have to regard the solution (62) is a “formal” one.

2.4.2. $l = 0$ Even-Mode Solution

On the other hand, for the

l = 0

-mode, we may choose

{\tilde{T}}_{(e 1) A} = 0

in Equations (53), (54), (56)–(61) with

l = 0

. Then, we derived the

l = 0

mode solution

\begin{matrix} F_{a b} & = & \frac{2}{r} (M_{1} + 4 π \int d r \frac{r^{2}}{f} T_{t t}) ({(d t)}_{a} {(d t)}_{a} + \frac{1}{f^{2}} {(d r)}_{a} {(d r)}_{a}) \\ + 2 [4 π r \int d t (\frac{1}{f} {\tilde{T}}_{t t} + f {\tilde{T}}_{r r})] {(d t)}_{(a} {(d r)}_{b)} + £_{V} g_{a b}, \end{matrix}

(65)

where

\begin{matrix} V_{a} = (\frac{f}{4} Υ + \frac{r f}{4} \partial_{r} Υ - \frac{r Ξ (r)}{(1 - 3 f)} + f \int d r \frac{2 Ξ (r)}{f {(1 - 3 f)}^{2}}) {(d t)}_{a} + \frac{1}{4 f} r \partial_{t} Υ {(d r)}_{a} . \end{matrix}

(66)

Here, the variable

\tilde{F} = : \partial_{t} Υ

must satisfy the equation

\begin{matrix} - \frac{1}{f} \partial_{t}^{2} Υ + \partial_{r} (f \partial_{r} Υ) + \frac{3 (1 - f)}{r^{2}} Υ - \frac{8}{r^{3}} \int d t m_{1} (t, r) - \frac{4}{1 - 3 f} \partial_{r} Ξ (r) \\ = & 16 π \int d t (- \frac{1}{f} {\tilde{T}}_{t t} + f {\tilde{T}}_{r r}), \end{matrix}

(67)

where

m_{1} (t, r)

is given by

\begin{matrix} m_{1} (t, r) = 4 π \int d r \frac{r^{2}}{f} {\tilde{T}}_{t t} + M_{1} = 4 π \int d t r^{2} f {\tilde{T}}_{t r} + M_{1}, \end{matrix}

(68)

M_{1}

is the constant corresponding to the Schwarzschild mass perturbation, and

Ξ (r)

is an arbitrary function of r.

3. Rule of Comparison and Gauge-Transformation Rules in a Conventional Gauge-Fixing

The main purpose of this paper is to check the following statement. “Gauge invariant formulations of perturbations are equivalent to complete gauge fixing approaches.” However, this statement is too ambiguous to check if we have the background knowledge explained in Sec. 2. For example, there is no explanation of the terminology “gauge” in this statement. Therefore, we have to clarify this statement as follows:

Our rule for comparison: First of all, we assume the terminology “gauge” in the statement “Gauge invariant formulations of perturbations are equivalent to complete gauge fixing approaches” is the second-kind gauge which is explained in Sec. 2.1. Therefore, the gauge-transformation rule for this statement is given by (4). Furthermore, the degree of freedom that changes under this gauge-transformation rule is regarded as “unphysical.” The “gauge fixing” in the above statement is a specification of some perturbative variables through the degree of freedom of the generator $ξ_{(1)}^{a}$ . Furthermore, “complete gauge fixing” in the above statement is a specification of some perturbative variables through the “entire” degree of freedom of the generator $ξ_{(1)}^{a}$ .

These are all rules of our game to compare our gauge-invariant formulation and a “conventional complete gauge-fixing approach” in which we use the spherical harmonics

Y_{l m}

from the starting point.

3.1. Metric Perturbations

Based on the above conceptual premise, we consider the metric perturbation

h_{a b}

on the background Schwarzschild spacetime

(M, g_{a b})

whose metric

g_{a b}

is given by Equations (15)–(19). We consider the components of the metric perturbation

h_{a b}

as Equation (20) and the decomposition of these components

{h_{A B}, h_{A p}, h_{p q}}

as Equations (26)–(28) but we concentrate on the case

S_{δ} = Y_{l m} = : S

, where

Y_{l m}

is the conventional spherical harmonics.

Since we choose

S = Y_{l m}

, we have

{\hat{D}}_{p} S

ϵ_{p q} {\hat{D}}^{q} S

= 0,

({\hat{D}}_{p} {\hat{D}}_{q} - \frac{1}{2} γ_{p q} {\hat{D}}^{r} {\hat{D}}_{r}) S

2 ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} S

= 0 for

l = 0

modes. For

l = 1

modes,

({\hat{D}}_{p} {\hat{D}}_{q} - \frac{1}{2} γ_{p q} {\hat{D}}^{r} {\hat{D}}_{r}) S

2 ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} S

= 0. Due to these facts, we cannot construct gauge-invariant variables for

l = 0, 1

modes in a similar manner to the derivation of Equations (36)–() for

l \geq 2

modes. Then, we cannot use the gauge-invariant formulation reviewed in Sec. 2. Instead, we have to fix the second-kind gauge degree of freedom to exclude the “unphysical” degree of freedom.

3.2. Conventional gauge-transformation rules for $l = 0, 1$ metric perturbations

Here, we consider the gauge-transformation rule

\begin{matrix} {}_{Y} h_{a b} - {}_{X} h_{a b} = £_{ξ} g_{a b} = 2 \nabla_{(a} ξ_{b)} . \end{matrix}

(69)

From this gauge-transformation rule, we can derive the gauge-transformation rule for the components

{h_{A B}, h_{A p}, h_{q p}}

defined by Equation (20) is given by

\begin{matrix} {}_{Y} h_{A B} - {}_{X} h_{A B} & = & £_{ξ} g_{A B} = \nabla_{A} ξ_{B} + \nabla_{B} ξ_{A} = {\bar{D}}_{A} ξ_{B} + {\bar{D}}_{B} ξ_{A}, \end{matrix}

(70)

\begin{matrix} {}_{Y} h_{A p} - {}_{X} h_{A p} & = & £_{ξ} g_{A p} = \nabla_{A} ξ_{p} + \nabla_{p} ξ_{A} = {\bar{D}}_{A} ξ_{p} + {\hat{D}}_{p} ξ_{A} - \frac{2}{r} ({\bar{D}}_{A} r) ξ_{p}, \end{matrix}

(71)

\begin{matrix} {}_{Y} h_{p q} - {}_{X} h_{p q} & = & £_{ξ} g_{p q} = \nabla_{p} ξ_{q} + \nabla_{q} ξ_{p} = {\hat{D}}_{p} ξ_{q} + {\hat{D}}_{q} ξ_{p} + 2 r ({\bar{D}}^{A} r) γ_{p q} ξ_{A} \end{matrix}

(72)

from the formulae summarized in Appendix B of the Part I paper [14]. Here, we consider the Fourier transformation of

ξ_{a} = : ξ_{A} {(d x^{A})}_{a} + ξ_{p} {(d x^{p})}_{a}

\begin{matrix} ξ_{A} = \sum_{l, m} ζ_{A} S, ξ_{p} = r \sum_{l, m} (ζ_{(e)} {\hat{D}}_{p} S + ζ_{(o)} ϵ_{p q} {\hat{D}}^{p} S) . \end{matrix}

(73)

From these Fourier transformation rules, Equations (70)–(72) are given by

\begin{matrix} {}_{Y} h_{A B} - {}_{X} h_{A B} & = & {\bar{D}}_{A} ξ_{B} + {\bar{D}}_{B} ξ_{A} = \sum_{l, m} 2 {\bar{D}}_{(A} ζ_{B)} S, \\ {}_{Y} h_{A p} - {}_{X} h_{A p} & = & {\bar{D}}_{A} ξ_{p} + {\hat{D}}_{p} ξ_{A} - \frac{2}{r} ({\bar{D}}_{A} r) ξ_{p} \\ = & r \sum_{l, m} [(\frac{1}{r} ζ_{A} + {\bar{D}}_{A} ζ_{(e)} - \frac{1}{r} ({\bar{D}}_{A} r) ζ_{(e)}) {\hat{D}}_{p} S \end{matrix}

(74)

\begin{matrix} + ({\bar{D}}_{A} ζ_{(o)} - \frac{1}{r} ({\bar{D}}_{A} r) ζ_{(o)}) ϵ_{p q} {\hat{D}}^{p} S], \\ {}_{Y} h_{p q} - {}_{X} h_{p q} & = & {\hat{D}}_{p} ξ_{q} + {\hat{D}}_{q} ξ_{p} + 2 r ({\bar{D}}^{A} r) γ_{p q} ξ_{A} \\ = & r^{2} \sum_{l, m} [\frac{4}{r} (- \frac{l (l + 1)}{2} ζ_{(e)} + ({\bar{D}}^{A} r) ζ_{A}) \frac{1}{2} γ_{p q} S \\ + \frac{2}{r} ζ_{(e)} ({\hat{D}}_{p} {\hat{D}}_{q} S - \frac{1}{2} γ_{p q} {\hat{D}}^{r} {\hat{D}}_{r} S) \end{matrix}

(75)

\begin{matrix} - \frac{1}{r} ζ_{(o)} 2 ϵ_{r (q} {\hat{D}}_{p)} {\hat{D}}^{r} S] . \end{matrix}

(76)

Here, we used the property of the mode function S is an eigen function of the Laplacian

{\hat{D}}_{r} {\hat{D}}^{r} : = γ^{r s} {\hat{D}}_{r} {\hat{D}}_{s}

\begin{matrix} {\hat{D}}_{r} {\hat{D}}^{r} S = - l (l + 1) S, S = Y_{l m} . \end{matrix}

(77)

3.2.1. $l \geq 2$ Perturbations

For

l \geq 2

modes, the set of mode functions

\begin{matrix} \{S, {\hat{D}}_{p} S, ϵ_{p q} {\hat{D}}^{q} S, \frac{1}{2} γ_{p q} S, ({\hat{D}}_{p} {\hat{D}}_{q} - \frac{1}{2} γ_{p q} {\hat{D}}_{r} {\hat{D}}^{r}) S, 2 ϵ_{r (p} {\hat{D}}^{r} {\hat{D}}_{q)} S\} \end{matrix}

(78)

is a linear-independent set of the tensor field of the rank 0, 1, and 2, even if

S = Y_{l m}

. Then, we may compare Equations (26)–() and Equations (74)–(). As the result of this comparison, we obtain the gauge-transformation rules for the mode functions

{{\tilde{h}}_{A B}, {\tilde{h}}_{(e 1) A}, {\tilde{h}}_{(o 1) A}, {\tilde{h}}_{(e 0)}, {\tilde{h}}_{(e 2)}, {\tilde{h}}_{(o 2)}}

\begin{matrix} {}_{Y}{\tilde{h}}_{A B} - {}_{X}{\tilde{h}}_{A B} & = & 2 {\bar{D}}_{(A} ζ_{B)}, \end{matrix}

(79)

\begin{matrix} {}_{Y}{\tilde{h}}_{(e 1) A} - {}_{X}{\tilde{h}}_{(e 1) A} & = & \frac{1}{r} ζ_{A} + {\bar{D}}_{A} ζ_{(e)} - \frac{1}{r} ({\bar{D}}_{A} r) ζ_{(e)}, \end{matrix}

(80)

\begin{matrix} {}_{Y}{\tilde{h}}_{(o 1) A} - {}_{X}{\tilde{h}}_{(o 1) A} & = & {\bar{D}}_{A} ζ_{(o)} - \frac{1}{r} ({\bar{D}}_{A} r) ζ_{(o)}, \end{matrix}

(81)

\begin{matrix} {}_{Y}{\tilde{h}}_{(e 0)} - {}_{X}{\tilde{h}}_{(e 0)} & = & \frac{4}{r} (- \frac{l (l + 1)}{2} ζ_{(e)} + ({\bar{D}}^{A} r) ζ_{A}), \end{matrix}

(82)

\begin{matrix} {}_{Y}{\tilde{h}}_{(e 2)} - {}_{X}{\tilde{h}}_{(e 2)} & = & \frac{2}{r} ζ_{(e)}, \end{matrix}

(83)

\begin{matrix} {}_{Y}{\tilde{h}}_{(o 2)} - {}_{X}{\tilde{h}}_{(o 2)} & = & - \frac{1}{r} ζ_{(o)} . \end{matrix}

(84)

From these gauge-transformation rules, it is well-known that we can construct gauge-invariant variables and the gauge-dependent variables and Conjecture 2.1 is valid for

l \geq 2

modes.

3.2.2. $l = 1$ Perturbations

As shown in the Appendix A in Ref. [14], for

l = 1

modes,

\begin{matrix} {\hat{D}}_{p} Y_{1 m} \neq 0 \neq ϵ_{p q} {\hat{D}}^{q} Y_{1 m} \end{matrix}

(85)

but

\begin{matrix} ({\hat{D}}_{p} {\hat{D}}_{q} - \frac{1}{2} {\hat{D}}_{r} {\hat{D}}^{r}) Y_{1 m} = 0 = 2 ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} Y_{1 m} . \end{matrix}

(86)

In this case, the Fourier transformation (26)–() of the metric perturbation with

S_{δ} = S = Y_{l m}

is given by

\begin{matrix} h_{A B} & = & \sum_{m} {\tilde{h}}_{A B} S, \end{matrix}

(87)

\begin{matrix} h_{A p} & = & \sum_{m} r {\tilde{h}}_{(e 1) A} {\hat{D}}_{p} S + \sum_{m} r {\tilde{h}}_{(o 1) A} ϵ_{p q} {\hat{D}}^{q} S, \end{matrix}

(88)

\begin{matrix} h_{p q} & = & \sum_{m} \frac{r^{2}}{2} γ_{p q} {\tilde{h}}_{(e 0)} S . \end{matrix}

(89)

The gauge-transformation rules (74)–(76) for each m mode are given by

\begin{matrix} {}_{Y} {\tilde{h}}_{A B} - {}_{X} {\tilde{h}}_{A B} & = & 2 {\bar{D}}_{(A} ζ_{B)}, \end{matrix}

(90)

\begin{matrix} {}_{Y} {\tilde{h}}_{(e 1) A} - {}_{X} {\tilde{h}}_{(e 1) A} & = & \frac{1}{r} ζ_{A} + {\bar{D}}_{A} ζ_{(e)} - \frac{1}{r} ({\bar{D}}_{A} r) ζ_{(e)}, \end{matrix}

(91)

\begin{matrix} {}_{Y} {\tilde{h}}_{(o 1) A} - {}_{X} {\tilde{h}}_{(o 1) A} & = & {\bar{D}}_{A} ζ_{(o)} - \frac{1}{r} ({\bar{D}}_{A} r) ζ_{(o)}, \end{matrix}

(92)

\begin{matrix} {}_{Y} {\tilde{h}}_{(e 0)} - {}_{X} {\tilde{h}}_{(e 0)} & = & - \frac{4}{r} ζ_{(e)} + \frac{4}{r} ({\bar{D}}^{A} r) ζ_{A} . \end{matrix}

(93)

Comparing the gauge-transformation rules (79)–(84) for

l \geq 2

with the gauge-transformation rules (90)–(93), it is easy to find the gauge-transformation rule (83) and (84) for

l \geq 2

do not appear in the

l = 1

mode gauge transformation. This is due to the fact Equations (86), and the reason why we cannot construct gauge-invariant variables for

l = 1

mode perturbations in a similar method to the

l \geq 2

case.

3.2.3. $l = 0$ Perturbations

The spherical harmonic function

S = Y_{l m}

is constant when

l = 0

. In this case, the Fourier transformation (26)–(28) of the metric perturbation with

S_{δ} = S = Y_{l m}

is given by

\begin{matrix} h_{A B} & = & {\tilde{h}}_{A B} S, \end{matrix}

(94)

\begin{matrix} h_{A p} & = & 0, \end{matrix}

(95)

\begin{matrix} h_{p q} & = & \frac{r^{2}}{2} γ_{p q} {\tilde{h}}_{(e 0)} S . \end{matrix}

(96)

The gauge-transformation rules (74)–() are given by

\begin{matrix} {}_{Y} {\tilde{h}}_{A B} - {}_{X} {\tilde{h}}_{A B} & = & 2 {\bar{D}}_{(A} ζ_{B)} = {\bar{D}}_{A} ζ_{B} + {\bar{D}}_{B} ζ_{A}, \end{matrix}

(97)

\begin{matrix} {}_{Y} {\tilde{h}}_{(e 0)} - {}_{X} {\tilde{h}}_{(e 0)} & = & \frac{4}{r} ({\bar{D}}^{A} r) ζ_{A} . \end{matrix}

(98)

It is easy to see that many gauge-transformation rules in (79)–(84) are missing. This is due to the fact

\begin{matrix} {\hat{D}}_{p} S = ϵ_{p q} {\hat{D}}^{q} S = 0, ({\hat{D}}_{q} {\hat{D}}_{p} - \frac{1}{2} γ_{p q} {\hat{D}}_{r} {\hat{D}}^{r}) S = 2 ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} S = 0 \end{matrix}

(99)

This is the reason why we cannot construct gauge-invariant variables for

l = 0

mode perturbations in a similar method to the

l \geq 2

case.

4. l=1 Odd-Mode Perturbation in the Conventional Approach

As discussed in Sec. 3.2.2,

l = 1

mode perturbations are given by Equations (87)–(89). In particular, among these expressions of the

l = 1

mode perturbation, odd-mode perturbation is given by

\begin{matrix} h_{A B} & = & 0, h_{A p} = r {\tilde{h}}_{(o 1) A} ϵ_{p q} {\hat{D}}^{q} S, h_{p q} = 0 . \end{matrix}

(100)

As the property of the

l = 1

spherical harmonics, we obtain the condition (86). For odd-mode perturbation we have

\begin{matrix} 2 ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} Y_{1 m} = 0 . \end{matrix}

(101)

Here, we apply the notation which is introduced by Equations (A14)–(A15) and we obtain

\begin{matrix} {\bar{h}}_{A B} = 0, {\bar{h}}_{A}^{D} = 0, {\bar{h}}^{p D} : = γ^{p q} y^{D E} r {\tilde{h}}_{(o 1) E} ϵ_{q r} {\hat{D}}^{r} S, {\bar{h}}_{p}^{q} = 0, {\bar{h}}^{p q} = 0, \end{matrix}

(102)

for

l = 1

odd mode perturbations. Through this notation of the metric perturbation, the linear perturbations (A16)–(A18) of the Einstein tensor are given by

\begin{matrix} {}^{(1)} G_{A}^{B} & = & 0, \end{matrix}

(103)

\begin{matrix} {}^{(1)} G_{A}^{q} & = & \frac{1}{2 r} [{\bar{D}}_{A} {\bar{D}}^{C} {\tilde{h}}_{(o 1) C} - {\bar{D}}_{C} {\bar{D}}^{C} {\tilde{h}}_{(o 1) A} - \frac{2}{r} ({\bar{D}}^{C} r) {\bar{D}}_{C} {\tilde{h}}_{(o 1) A} \\ + \frac{3}{r} ({\bar{D}}^{C} r) {\bar{D}}_{A} {\tilde{h}}_{(o 1) C} - \frac{1}{r} ({\bar{D}}_{A} r) {\bar{D}}^{C} {\tilde{h}}_{(o 1) C} + \frac{1}{2 r^{2}} ({\bar{D}}_{C} r) ({\bar{D}}^{C} r) {\tilde{h}}_{(o 1) A} \\ - \frac{2}{r^{2}} ({\bar{D}}_{A} r) ({\bar{D}}^{C} r) {\tilde{h}}_{(o 1) C} + \frac{3}{2 r^{2}} {\tilde{h}}_{(o 1) A}] ϵ^{q r} {\hat{D}}_{r} S, \end{matrix}

(104)

\begin{matrix} {}^{(1)} G_{p}^{q} & = & - \frac{1}{2 r^{2}} {\bar{D}}^{C} (r {\tilde{h}}_{(o 1) C}) γ^{q r} 2 ϵ_{s (p} {\hat{D}}_{r)} {\hat{D}}^{s} S = 0 . \end{matrix}

(105)

The final equality in Equation (105) is due to the property of the spherical harmonics

Y_{l m}

(101). Furthermore, the expression (104) is gauge invariant under the gauge transformation rule (). On the other hand, the

{\bar{D}}^{C} (r {\tilde{h}}_{(o 1) C})

in Equation (105) is not gauge invariant as shown in below. However, the gauge-invariance of the linear-order Einstein tensor

{}^{(1)} G_{a}^{b}

is guaranteed by the identity

2 ϵ_{s (p} {\hat{D}}_{r)} {\hat{D}}^{s} S = 0

for the

l = 1

odd-mode perturbations.

For the

l = 1

odd-mode perturbations, the components of the linearized energy-momentum tensor are summarized as

\begin{matrix} {}^{(1)} T_{A}^{B} = 0, {}^{(1)} T_{A}^{q} = \frac{1}{r} {\tilde{T}}_{(o 1) A} ϵ^{q r} {\hat{D}}_{r} S, {}^{(1)} T_{p}^{q} = 0 . \end{matrix}

(106)

Then, the linearized Einstein equations for the odd-mode perturbations are given by

\begin{matrix} {\bar{D}}_{A} {\bar{D}}^{C} {\tilde{h}}_{(o 1) C} - {\bar{D}}_{C} {\bar{D}}^{C} {\tilde{h}}_{(o 1) A} \\ - \frac{2}{r} ({\bar{D}}^{C} r) {\bar{D}}_{C} {\tilde{h}}_{(o 1) A} + \frac{3}{r} ({\bar{D}}^{C} r) {\bar{D}}_{A} {\tilde{h}}_{(o 1) C} - \frac{1}{r} ({\bar{D}}_{A} r) {\bar{D}}^{C} {\tilde{h}}_{(o 1) C} \\ + \frac{1}{2 r^{2}} ({\bar{D}}_{C} r) ({\bar{D}}^{C} r) {\tilde{h}}_{(o 1) A} - \frac{2}{r^{2}} ({\bar{D}}_{A} r) ({\bar{D}}^{C} r) {\tilde{h}}_{(o 1) C} + \frac{3}{2 r^{2}} {\tilde{h}}_{(o 1) A} \\ = & 16 π {\tilde{T}}_{(o 1) A}, \end{matrix}

(107)

Although the equation

\begin{matrix} {\bar{D}}^{C} (r {\tilde{h}}_{(o 1) C}) = 0 \end{matrix}

(108)

does not appear from Equation (105) due to the fact that

2 ϵ_{s (p} {\hat{D}}_{r)} {\hat{D}}^{s} Y_{1 m} = 0

, we may use Equation (108) as a gauge condition. As noted in Sec. 3.2.2, the gauge-transformation rule for the variable

{\tilde{h}}_{(o 1) C}

is given by Equation (92). From the gauge transformation rule (92), we consider the gauge-transformation rule for the left-hand side of Equation (108) as

\begin{matrix} {\bar{D}}^{A} (r {}_{Y} {\tilde{h}}_{(o 1) A}) - {\bar{D}}^{A} (r {}_{X} {\tilde{h}}_{(o 1) A}) & = & r {\bar{D}}^{A} {\bar{D}}_{A} ζ_{(o)} - ({\bar{D}}^{A} {\bar{D}}_{A} r) ζ_{(o)} . \end{matrix}

(109)

Using the background Einstein equation (Equation (B67) of Appendix B in Ref. [14]), we consider the equation

\begin{matrix} r {\bar{D}}^{C} {\bar{D}}_{C} ζ_{(o)} - \frac{1}{r} (1 - ({\bar{D}}^{C} r) ({\bar{D}}_{C} r)) ζ_{(o)} = - {\bar{D}}^{C} (r {}_{X} {\tilde{h}}_{(o 1) C}) \end{matrix}

(110)

More explicitly, Equation (110)

\begin{matrix} - \partial_{t}^{2} ζ_{(o)} + f \partial_{r} (f \partial_{r} ζ_{(o)}) - \frac{f}{r^{2}} (1 - f) ζ_{(o)} = - \frac{f}{r} {\bar{D}}^{C} (r {}_{X} {\tilde{h}}_{(o 1) C}) \end{matrix}

(111)

If we choose

ζ_{(o)}

as a special solution to Equation (111) or equivalently Equation (110), Equation (108) is regarded as a gauge condition in the

Y

-gauge, i.e.,

\begin{matrix} {\bar{D}}^{C} (r {}_{Y} {\tilde{h}}_{(o 1) C}) & = & 0 . \end{matrix}

(112)

We have to emphasize that this is not a complete gauge fixing, since there is a room of the choice of

ζ_{(o)}

which satisfy the homogeneous equation of Equation (110):

\begin{matrix} r {\bar{D}}^{C} {\bar{D}}_{C} ζ_{(o)} - \frac{1}{r} (1 - ({\bar{D}}^{C} r) ({\bar{D}}_{C} r)) ζ_{(o)} = 0, \end{matrix}

(113)

i.e.,

\begin{matrix} - \partial_{t}^{2} ζ_{(o)} + f \partial_{r} (f \partial_{r} ζ_{(o)}) - \frac{f}{r^{2}} (1 - f) ζ_{(o)} = 0 . \end{matrix}

(114)

Under the gauge choice (112), Equation (107) is given by

\begin{matrix} [{\bar{D}}_{C} {\bar{D}}^{C} - \frac{2}{r^{2}}] (r {\tilde{h}}_{(o 1) A}) - \frac{2}{r^{2}} ({\bar{D}}_{A} r) ({\bar{D}}^{C} r) (r {\tilde{h}}_{(o 1) C}) + \frac{2}{r} ({\bar{D}}^{C} r) {\bar{D}}_{A} (r {\tilde{h}}_{(o 1) C}) \\ = & 16 π r {\tilde{T}}_{(o 1) A} . \end{matrix}

(115)

Although the variable

r {\tilde{h}}_{(o 1) C}

is a gauge-dependent variable which is different from the gauge-invariant variable

r {\tilde{F}}_{A}

, we can obtain the equation (115) if we replace the variable

r {\tilde{F}}_{A}

in Equation (47) with the variable

r {\tilde{h}}_{(o 1) C}

We also note that the gauge condition (112) coincides with Equation (46), though we have to replace the gauge-invariant variable

r {\tilde{F}}^{D}

with the gauge-dependent variable

r {\tilde{h}}_{(o 1) C}

in Equation (46) to confirm this coincidence. Furthermore, we also take into account the continuity equation (48) of the

l = 1

odd-mode perturbation of the energy-momentum tensor. Thus, the equations to be solved for the

l = 1

odd-mode perturbation are the gauge condition (108), the evolution equation (115), and the continuity equation (48). These equations coincide with Equations (46)–(48) except for the fact that the variable to be obtained is not the gauge-invariant

r {\tilde{F}}^{D}

variable but the gauge-dependent variable

r {\tilde{h}}_{(o 1) C}

. Then, through the same logic in Ref. [14], we obtain the solution to the gauge condition (112), the evolution equation (115), and the continuity equation (48) as follows:

\begin{matrix} 2 r {\tilde{h}}_{(o 1) C} {sin}^{2} θ {(d x^{C})}_{(a} {(d ϕ)}_{b)} = 6 M r^{2} [\int d r \frac{a_{1} (t, r)}{r^{4}}] {sin}^{2} θ {(d t)}_{(a} {(d ϕ)}_{b)} \end{matrix}

\begin{matrix} + £_{V} g_{a b},, \end{matrix}

(116)

\begin{matrix} V_{a} = (β_{1} t + β_{0} + W_{(o)} (t, r)) r^{2} {sin}^{2} θ {(d ϕ)}_{a}, \end{matrix}

(117)

Here, we concentrate only on the

m = 0

solution,

β_{1}

and

β_{0}

are constant, and

Z_{(o)} = r f \partial_{r} W_{(o)} (t, r)

is an arbitrary function which satisfies the equation

\begin{matrix} \partial_{t}^{2} Z_{(o)} - f \partial_{r} (f \partial_{r} Z_{(o)}) + \frac{1}{r^{2}} f [2 - 3 (1 - f)] Z_{(o)} = 16 π f^{2} {\tilde{T}}_{(o 1) r} . \end{matrix}

(118)

a_{1} (t, r)

in Equation (116) is given by Equation (6.44) in Ref. [14], i.e.,

\begin{matrix} a_{1} (t, r) & = & - \frac{16 π}{3 M} r^{3} f \int d t {\tilde{T}}_{(o 1) r} + a_{10} \\ = & - \frac{16 π}{3 M} \int d r r^{3} \frac{1}{f} {\tilde{T}}_{(o 1) t} + a_{10}, \end{matrix}

(119)

where

a_{10}

is the perturbative Kerr parameter.

Note that the formal solution described by Equations (116)–(119) has the same form as the formal solution described by Equations (49)–(52). However, we have to emphasize that the variable

F_{A p}

in Equation (49) is gauge invariant as noted by Equation (43) and the vector field

V_{a}

in Equation (49) is also gauge invariant. On the other hand, the variable

{\tilde{h}}_{(o 1) C}

is still gauge-dependent. Actually, there are remaining gauge degrees of freedom of the generator

ζ_{(o)}

which satisfy Equation (114) as noted above. This is clear from the fact that the gauge transformation rule (92) with Equation (114) gives a still non-trivial transformation rule. This remaining gauge degree of freedom is so-called “residual gauge”. For this reason, there is a possibility that

V_{a}

in Equation (116) includes this residual gauge.

To clarify whether

V_{a}

in Equation (116) includes the “residual gauge”, we have to confirm Equation (114). Within our rules to compare our gauge-invariant formulation with a conventional gauge-fixed approach, we regard the terms in

V_{a}

in Equation (116) which satisfies Equation (114) is the second-kind gauge degree of freedom and we regard these degrees of freedom as “unphysical degree of freedom.” To clarify this “unphysical degree of freedom,” we introduce the indicator function

R_{(o)} [*]

\begin{matrix} R_{(o)} [ζ_{(o)}] : = - \partial_{t}^{2} ζ_{(o)} + f \partial_{r} (f \partial_{r} ζ_{(o)}) - \frac{f}{r^{2}} (1 - f) ζ_{(o)} . \end{matrix}

(120)

R_{(o)} [ζ_{(o)}] = 0

, we should regard

ζ_{(o)}

is the second-kind gauge and we regard

ζ_{(o)}

as “unphysical degree of freedom.”

We can easily confirm that

\begin{matrix} R_{(o)} [(β_{1} t + β_{0}) r] = 0 . \end{matrix}

(121)

Then, according to our above rule of comparison, we have to conclude that the rigid rotating term

(β_{1} t + β_{0}) r

V_{a}

in Equation (117) should be regarded as the second-kind gauge degree of freedom which is “unphysical degree of freedom.”

Next, we consider the term

W_{(o)} (t, r) r

in Equation (117). In this case, the direct calculation of the indicator

R_{(o)} [W_{(o)} (t, r) r]

is useless. However, it is useful to consider the r-derivative of

R_{(o)} [W_{(o)} (t, r) r]

and we can show that

\begin{matrix} r f \partial_{r} (\frac{1}{r} R_{(o)} [W_{(o)} (t, r) r]) & = & - \partial_{t}^{2} Z_{(o)} + f \partial_{r} (f \partial_{r} Z_{(o)}) - \frac{f}{r^{2}} (2 - 3 (1 - f)) Z_{(o)}, \end{matrix}

(122)

where we used

Z_{(o)} = r f \partial_{r} W_{(o)} (t, r)

. Since the left-hand side of Equation (122) coincides with the right-hand side of Equation (118). Through Equation (118), we obtain

\begin{matrix} r f \partial_{r} (\frac{1}{r} R_{(o)} [W_{(o)} (t, r) r]) & = & - 16 π f^{2} {\tilde{T}}_{(o 1) r} . \end{matrix}

(123)

or, equivalently,

\begin{matrix} R_{(o)} [W_{(o)} (t, r) r] & = & - 16 π r \int d r \frac{f}{r} {\tilde{T}}_{(o 1) r} . \end{matrix}

(124)

Then, if we consider the case where

{\tilde{T}}_{(o 1) r} \neq 0

, we have nonvanishing

R_{(o)} [W_{(o)} (t, r) r]

. This means that the

W_{(o)} (t, r)

term does not belong to the second-kind gauge, and we have to regard the degree of freedom

W_{(o)} (t, r)

in Equation (117) is a “physical one”.

On the other hand, even in the case where

{\tilde{T}}_{(o 1) r} = 0

, Equation (122) is valid. If

W_{(o)} (t, r)

belongs to the second-kind gauge, i.e.,

R_{(o)} [W_{(o)} (t, r) r] = 0

, Equation (122) yields

\begin{matrix} - \partial_{t}^{2} Z_{(o)} + f \partial_{r} (f \partial_{r} Z_{(o)}) - \frac{f}{r^{2}} (2 - 3 (1 - f)) Z_{(o)} = 0 . \end{matrix}

(125)

However, even if

Z_{(o)}

is a solution to Equation (125), we cannot directly yield

R_{(o)} [W_{(o)} (t, r) r] = 0

. Therefore, considering the following two sets of function

W_{(o)} (t, r) r

\begin{matrix} G_{(o)} & : = & \{r W_{(o)} (t, r)| R_{(o)} [W_{(o)} (t, r) r] = 0\}, \\ H_{(o)} & : = & \{r W_{(o)} (t, r)| Z_{(o)} = r f \partial_{r} W_{(o)} (t, r), \end{matrix}

(126)

\begin{matrix} - \partial_{t}^{2} Z_{(o)} + f \partial_{r} (f \partial_{r} Z_{(o)}) - \frac{f}{r^{2}} (2 - 3 (1 - f)) Z_{(o)} = 0 .\}, \end{matrix}

(127)

we obtain the relation

\begin{matrix} G_{(o)} \subset H_{(o)} . \end{matrix}

(128)

This indicates that a part of solutions to Equation (125) should be regarded as a gauge degree of freedom of the second kind which is the “unphysical degree of freedom.”

Furthermore, to obtain the explicit solution

W_{(o)} (t, r)

, we have to solve Equation (118) with appropriate boundary conditions. Equation (118) is an inhomogeneous second-order linear differential equation for

Z_{(o)}

and its boundary conditions are adjusted by the homogeneous solutions to Equation (118), i.e., the element of the set of function

H_{(o)}

. However, a part of this homogeneous solution to Equation (118) should be regarded as an unphysical degree of freedom in the “complete gauge fixing approach” as mentioned above. Therefore, in the conventional “complete gauge fixing approach”, the boundary conditions for Equation (118) is restricted. In this sense, a conventional “complete gauge-fixing approach” includes a stronger restriction than our proposed gauge-invariant formulation.

5. l=1 Even-Mode Perturbation in the Conventional Approach

As discussed in Sec. 3.2.2,

l = 1

mode perturbations are given by Equations (87)–(89). In particular, among these expressions of the

l = 1

mode perturbations, even-mode perturbation is given by

\begin{matrix} h_{A B} = {\tilde{h}}_{A B} S, h_{A p} = r {\tilde{h}}_{(e 1) A} {\hat{D}}_{p} S, h_{p q} = \frac{r^{2}}{2} γ_{p q} {\tilde{h}}_{(e 0)} S . \end{matrix}

(129)

As the property of the

l = 1

spherical harmonics, we obtain the condition (86). For even-mode perturbation, we have

\begin{matrix} ({\hat{D}}_{p} {\hat{D}}_{q} - \frac{1}{2} γ_{p q} {\hat{D}}_{r} {\hat{D}}^{r}) Y_{1 m} = 0 . \end{matrix}

(130)

The gauge-transformation rules for the

l = 1

even-mode perturbations are given by Equations (90), (91), and (93). Inspecting the gauge-transformation rules (91) and (93), we define the variable

\tilde{H}

\begin{matrix} \tilde{H} & : = & {\tilde{h}}_{(e 0)} - 4 ({\bar{D}}^{A} r) {\tilde{h}}_{(e 1) A} . \end{matrix}

(131)

The gauge-transformation rule of

\tilde{H}

is given by

\begin{matrix} {}_{Y} \tilde{H} - {}_{X} \tilde{H} & = & - 4 ({\bar{D}}^{A} r) {\bar{D}}_{A} ζ_{(e)} - \frac{4}{r} (1 - ({\bar{D}}^{A} r) ({\bar{D}}_{A} r)) ζ_{(e)} . \end{matrix}

(132)

Furthermore, inspecting gauge-transformation rules (90) and () we also define the variable

{\tilde{H}}_{A B}

\begin{matrix} {\tilde{H}}_{A B} & : = & {\tilde{h}}_{A B} - {\bar{D}}_{A} (r {\tilde{h}}_{(e 1) B}) - {\bar{D}}_{B} (r {\tilde{h}}_{(e 1) A}) . \end{matrix}

(133)

The gauge-transformation of

{\tilde{H}}_{A B}

is given by

\begin{matrix} {}_{Y} {\tilde{H}}_{A B} - {}_{X} {\tilde{H}}_{A B} & = & - 2 r {\bar{D}}_{A} {\bar{D}}_{B} ζ_{(e)} + 2 ({\bar{D}}_{A} {\bar{D}}_{B} r) ζ_{(e)} . \end{matrix}

(134)

The definitions (131) and (133) of the variables

\tilde{H}

and

{\tilde{H}}_{A B}

, respectively, are analogous to the gauge-invariant variable

\tilde{F}

and

{\tilde{F}}_{A B}

define by Equations (36) and (38) for

l \geq 2

modes, respectively. However, the variables

\tilde{H}

and

{\tilde{H}}_{A B}

are not gauge invariant. The employment of the variables

\tilde{H}

and

{\tilde{H}}_{A B}

corresponds to the gauge fixing of the gauge degree of freedom of the generator

ζ_{A}

and the specification of the component

{\tilde{h}}_{(e 1) A}

of the metric perturbation. On the other hand, the gauge-transformation rules (90), (91), and (93) includes the gauge degree of freedom of the generator

ζ_{(e)}

. This gauge degree of freedom appears in the gauge-transformation rules (132) and (134).

The linearized Einstein tensor for

l = 1

even modes in terms of

{\tilde{H}}_{A B}

and

\tilde{H}

are given as

\begin{matrix} y_{C B} {}^{(1)} G_{A}^{C} / S & = & [- \frac{1}{2} {\bar{D}}_{C} {\bar{D}}^{C} + \frac{3}{r^{2}} - \frac{1}{r} ({\bar{D}}^{C} r) {\bar{D}}_{C}] {\tilde{H}}_{A B} + {\bar{D}}_{(A} {\bar{D}}^{C} {\tilde{H}}_{B) C} - \frac{1}{2} {\bar{D}}_{A} {\bar{D}}_{B} {\tilde{H}}_{C}^{C} \\ + \frac{2}{r} ({\bar{D}}^{C} r) [{\bar{D}}_{(A} {\tilde{H}}_{B) C} - \frac{1}{r} ({\bar{D}}_{C} r) {\tilde{H}}_{A B}] - \frac{1}{2} {\bar{D}}_{A} {\bar{D}}_{B} \tilde{H} - \frac{1}{r} ({\bar{D}}_{(A} r) {\bar{D}}_{B)} \tilde{H} \\ + \frac{1}{2} y_{A B} [[{\bar{D}}_{C} {\bar{D}}^{C} + \frac{3}{r} ({\bar{D}}^{C} r) {\bar{D}}_{C}] \tilde{H} + \{{\bar{D}}_{D} {\bar{D}}^{D} - \frac{5}{r^{2}}\} {\tilde{H}}_{C}^{C} \\ + \frac{1}{r} ({\bar{D}}^{C} r) \{2 {\bar{D}}_{C} {\tilde{H}}_{D}^{D} + \frac{3}{r} ({\bar{D}}_{C} r) {\tilde{H}}_{D}^{D}\} - {\bar{D}}^{C} {\bar{D}}^{D} {\tilde{H}}_{C D} \\ - \frac{2}{r} ({\bar{D}}^{D} r) \{2 {\bar{D}}^{C} {\tilde{H}}_{C D} + \frac{1}{r} ({\bar{D}}^{C} r) {\tilde{H}}_{C D}\}], \end{matrix}

(135)

\begin{matrix} {}^{(1)} G_{A}^{q} & = & [\frac{1}{2 r^{2}} {\bar{D}}^{C} {\tilde{H}}_{A C} - \frac{1}{2 r^{2}} {\bar{D}}_{A} {\tilde{H}}_{C}^{C} + \frac{1}{2 r^{3}} ({\bar{D}}_{A} r) {\tilde{H}}_{C}^{C} - \frac{1}{4 r^{2}} {\bar{D}}_{A} \tilde{H}] {\hat{D}}^{q} S, \end{matrix}

(136)

\begin{matrix} γ_{q r} {}^{(1)} G_{p}^{r} & = & [+ \frac{1}{4} {\bar{D}}_{C} {\bar{D}}^{C} \tilde{H} + \frac{1}{2 r} ({\bar{D}}^{C} r) {\bar{D}}_{C} \tilde{H} + \frac{1}{2} \{+ {\bar{D}}_{C} {\bar{D}}^{C} + \frac{1}{r} ({\bar{D}}^{C} r) {\bar{D}}_{C} - \frac{1}{r^{2}}\} {\tilde{H}}_{D}^{D} \\ - \frac{1}{2} \{{\bar{D}}_{C} + \frac{2}{r} ({\bar{D}}_{C} r)\} {\bar{D}}_{D} {\tilde{H}}^{C D}] γ_{p q} S \\ - \frac{1}{2 r^{2}} {\tilde{H}}_{C}^{C} ({\hat{D}}_{p} {\hat{D}}_{q} S - \frac{1}{2} γ_{p q} {\hat{D}}^{r} {\hat{D}}_{r} S) . \end{matrix}

(137)

Since there is the identity (130) for

l = 1

mode perturbations, the last term of Equation (137) does not appear for

l = 1

even modes. Furthermore, the expressions (135) and (136) are gauge invariant under the gauge-transformation rules (132) and (134). Even in Equation (137) the component

γ_{q r} {}^{(1)} G_{p}^{r}

is gauge invariant except for the last term in Equation (137). Actually, the variable

{\tilde{H}}_{C}^{C}

is gauge dependent as shown below. However, the gauge-invariance

γ_{q r} {}^{(1)} G_{p}^{r}

is guaranteed by the identity (130).

On the other hand, the

l = 1

even components of them are given by

\begin{matrix} {}^{(1)} T_{A}^{B} & = & S {\tilde{T}}_{A}^{B}, \end{matrix}

(138)

\begin{matrix} γ_{q r} {}^{(1)} T_{A}^{r} & = & \frac{1}{r} {\tilde{T}}_{(e 1) A} {\hat{D}}_{q} S, \end{matrix}

(139)

\begin{matrix} γ_{q r} {}^{(1)} T_{p}^{r} & = & {\tilde{T}}_{(e 0)} \frac{1}{2} γ_{p q} S + {\tilde{T}}_{(e 2)} ({\hat{D}}_{p} {\hat{D}}_{q} S - \frac{1}{2} γ_{p q} {\hat{D}}_{r} {\hat{D}}^{r} S) \end{matrix}

(140)

Here again, we note that Equation (130) satisfies as a mathematical identity for

l = 1

mode perturbations. Therefore, the last term of Equation (140) does not appear for

l = 1

even modes.

If equation (130) is not satisfied, we have the equation

\begin{matrix} [- \frac{1}{2 r^{2}} {\tilde{H}}_{C}^{C}] ({\hat{D}}_{p} {\hat{D}}_{q} S - \frac{1}{2} γ_{p q} {\hat{D}}^{r} {\hat{D}}_{r} S) = 8 π {\tilde{T}}_{(e 2)} ({\hat{D}}_{p} {\hat{D}}_{q} S - \frac{1}{2} γ_{p q} {\hat{D}}_{r} {\hat{D}}^{r} S) \end{matrix}

(141)

as one of the components of the linearized Einstein equation. However, Equation (130) implies that this equation is identically satisfied. Therefore, this equation does not restrict

{\tilde{H}}_{C}^{C}

nor

{\tilde{T}}_{(e 2)}

and there is no other restriction of them. Here, we note that the tensor field

{\tilde{H}}_{A B}

is not gauge-invariant as shown in Equation (134). Since we may freely choose

{\tilde{H}}_{C}^{C}

and

{\tilde{T}}_{(e 2)}

, we choose

{\tilde{T}}_{(e 2)} = 0

by hand and choose

\begin{matrix} H_{C}^{C} = 0 . \end{matrix}

(142)

as a gauge condition.

Actually, from the gauge-transformation rule (134), we obtain

\begin{matrix} y^{A B} {}_{Y} {\tilde{H}}_{A B} - y^{A B} {}_{X} {\tilde{H}}_{A B} & = & - 2 r [- \frac{1}{f} \partial_{t}^{2} ζ_{(e)} + \partial_{r} (f \partial_{r} ζ_{(e)}) - \frac{1 - f}{r^{2}} ζ_{(e)}] . \end{matrix}

(143)

Then, if we choose

ζ_{(e)}

as a special solution to the equation

\begin{matrix} \frac{1}{2 r} y^{A B} {}_{X} {\tilde{H}}_{A B} & = & - \frac{1}{f} \partial_{t}^{2} ζ_{(e)} + \partial_{r} (f \partial_{r} ζ_{(e)}) - \frac{1 - f}{r^{2}} ζ_{(e)}, \end{matrix}

(144)

we may regard that

{}_{Y} {\tilde{H}}_{C}^{C} = 0

in the

Y

-gauge. We have to note that this gauge fixing (143) is not complete gauge fixing. There is a remaining degree of freedom in the choice of

ζ_{(e)}

as the homogeneous solution

ζ_{(e) h}

to the wave equation

\begin{matrix} - \frac{1}{f} \partial_{t}^{2} ζ_{(e) h} + \partial_{r} (f \partial_{r} ζ_{(e) h}) - \frac{1 - f}{r^{2}} ζ_{(e) h} = 0 . \end{matrix}

(145)

Due to the gauge condition (142), the components (135)–(137) of the linearized Einstein tensor and components (138)–(140) of the linear-order energy-momentum tensor yield the linearized Einstein equations. The

(A, p)

-components (equivalently,

(p, B)

-components) of the linearized Einstein equations are given by

\begin{matrix} {\bar{D}}^{C} {\tilde{H}}_{A C} - \frac{1}{2} {\bar{D}}_{A} \tilde{H} = 16 π r {\tilde{T}}_{(e 1) A} . \end{matrix}

(146)

Since the tensor

{\tilde{H}}_{A C}

is traceless due to the gauge condition (142), equation (146) coincides with Equation (54).

From the trace part of the

(p, q)

-component of the linearized Einstein equation and Equation (146) yields the component (61) of the continuity equation of the linearized energy-momentum tensor.

The trace part of

(A, B)

-component of the linearized Einstein equation with Equation (146) gives

\begin{matrix} {\bar{D}}_{C} {\bar{D}}^{C} \tilde{H} + \frac{2}{r} ({\bar{D}}_{C} r) {\bar{D}}^{C} \tilde{H} - \frac{4}{r^{2}} ({\bar{D}}^{C} r) ({\bar{D}}^{D} r) {\tilde{H}}_{C D} = 16 π ({\tilde{T}}_{C}^{C} + 4 ({\bar{D}}^{D} r) {\tilde{T}}_{(e 1) D}) . \end{matrix}

(147)

Since

{\tilde{H}}_{C D}

is a traceless tensor, Equation (147) coincides with the

l = 1

version of Equation (56) with the source term (57). However, we have to emphasize that

\tilde{H}

nor

{\tilde{H}}_{C D}

are not gauge invariant as shown above.

Finally, the traceless part of

(A, B)

-component of the linearized Einstein equation with Equations (146) and (147) yields

\begin{matrix} [- {\bar{D}}_{C} {\bar{D}}^{C} - \frac{2}{r} ({\bar{D}}^{C} r) {\bar{D}}_{C} + \frac{4}{r} ({\bar{D}}^{C} {\bar{D}}_{C} r) + \frac{2}{r^{2}}] {\tilde{H}}_{A B} + \frac{4}{r} ({\bar{D}}^{C} r) {\bar{D}}_{(A} {\tilde{H}}_{B) C} \\ - \frac{2}{r} ({\bar{D}}_{(A} r) {\bar{D}}_{B)} \tilde{H} \\ = & 16 π [{\tilde{T}}_{A B} - \frac{1}{2} y_{A B} {\tilde{T}}_{C}^{C} - 2 ({\bar{D}}_{(A} (r {\tilde{T}}_{(e 1) B)}) - \frac{1}{2} y_{A B} {\bar{D}}^{C} (r {\tilde{T}}_{(e 1) C})) \\ + 2 y_{A B} ({\bar{D}}^{D} r) {\tilde{T}}_{(e 1) D}], \end{matrix}

(148)

Since the variable

H_{A B}

is traceless due to the gauge condition (142), Equation (148) coincides with the

l = 1

version of Equation (58) with the source term (59).

In addition to these linearized Einstein equations, the following linearized perturbations of the continuity equation should be satisfied

\begin{matrix} {\bar{D}}^{C} {\tilde{T}}_{C}^{B} + \frac{2}{r} ({\bar{D}}^{D} r) {\tilde{T}}_{D}^{B} - \frac{2}{r} {\tilde{T}}_{(e 1)}^{B} - \frac{1}{r} ({\bar{D}}^{B} r) {\tilde{T}}_{(e 0)} = 0, \end{matrix}

(149)

\begin{matrix} {\bar{D}}^{C} {\tilde{T}}_{(e 1) C} + \frac{3}{r} ({\bar{D}}^{C} r) {\tilde{T}}_{(e 1) C} + \frac{1}{2 r} {\tilde{T}}_{(e 0)} = 0 . \end{matrix}

(150)

Together with the gauge condition (142), Equations (146)–() coincide with Equations (53)–(61) with

l = 1

in our gauge-invariant formulation developed in Refs. [12,13,14,15,16]. In Ref. [15], we derived the formal solution to Equations (53)–(61) with

l = 1

as Equation (62) with Equations (63), (64), and

m = 0

. Due to the coincidence of the set of equations, this formal solution should be the

m = 0

formal solution to Equations (142), and Equations (146)–(150). Then, as the

m = 0

solution, we obtain

\begin{matrix} H_{a b} & : = & H_{A B} cos θ {(d x^{A})}_{(a} {(d x^{B})}_{b)} + \frac{r^{2}}{2} H cos θ γ_{a b} \\ = & £_{V} g_{a b} - \frac{16 π r^{2}}{3 (1 - f)} [f^{2} \{\frac{1 + f}{2} {\tilde{T}}_{r r} + r f \partial_{r} {\tilde{T}}_{r r} - {\tilde{T}}_{(e 0)} - 4 {\tilde{T}}_{(e 1) r}\} {(d t)}_{a} {(d t)}_{b} \\ + \frac{2 r}{f} \{\partial_{t} {\tilde{T}}_{t t} - \frac{3 f (1 - f)}{2 r} {\tilde{T}}_{t r}\} {(d t)}_{(a} {(d r)}_{b)} \\ + \frac{r}{f} \{\partial_{r} {\tilde{T}}_{t t} - \frac{3 (1 - 3 f)}{2 r f} {\tilde{T}}_{t t}\} {(d r)}_{a} {(d r)}_{b}) \\ + r^{2} {\tilde{T}}_{t t} γ_{a b}] cos θ, \end{matrix}

(151)

where

γ_{a b} = γ_{p q} {(d x^{p})}_{a} {(d x^{q})}_{b}

V_{a} = g_{a b} V^{b}

is the vector field defined by

\begin{matrix} V_{a} : = - r \partial_{t} Φ_{(e)} cos θ {(d t)}_{a} + (Φ_{(e)} - r \partial_{r} Φ_{(e)}) cos {(d r)}_{a} - r Φ_{(e)} sin θ {(d θ)}_{a} \end{matrix}

(152)

and

Φ_{(e)}

is a solution to the equation

\begin{matrix} - \frac{1}{f} \partial_{t}^{2} Φ_{(e)} + \partial_{r} [f \partial_{r} Φ_{(e)}] - \frac{1 - f}{r^{2}} Φ_{(e)} = \frac{16 π r}{3 (1 - f)} S_{(Φ_{(e)})}, \end{matrix}

(153)

\begin{matrix} S_{(Φ_{(e)})} = \frac{1}{2} r \partial_{t} T_{t r} - \frac{1}{2} r \partial_{r} {\tilde{T}}_{t t} + \frac{1 - 4 f}{2 f} {\tilde{T}}_{t t} - \frac{f}{2} {\tilde{T}}_{r r} - f {\tilde{T}}_{(e 1) r} . \end{matrix}

(154)

As in the case of the

l = 1

odd-mode perturbation, the tensor field

F_{a b}

in Equation (62) is gauge invariant. Then,

V_{a}

in Equation (62), which defined by Equation (63) is also gauge invariant. Therefore, we regarded

V_{a}

in Equation (62) as the first kind gauge. On the other hand, the tensor field

H_{a b}

in Equation (151) is gauge-dependent in the sense of the second kind due to the gauge-transformation rules (132) and (134) for the components

\tilde{H}

and

{\tilde{H}}_{A B}

, respectively. Actually, there is a remaining gauge degree of freedom of the generator

ζ_{(e)}

which satisfies Equation (145) as noted above. This remaining gauge degree of freedom is so-called “residual gauge”. For this reason, there is a possibility that

V_{a}

in Equation (151) includes this “residual gauge”, while

V_{a}

in Equation (62) is gauge invariant.

Since we already fixed the gauge-degree of freedom

ζ_{(e)}

so that Equation (142) is satisfied, the remaining gauge degree of freedom

ζ_{(e) h}

must satisfy the equation (145). Therefore, to clarify whether

V_{a}

in Equation (151) includes the “residual gauge,” we have to confirm Equation (145). Within our rules to compare our gauge-invariant formulation with a conventional gauge-fixed approach, we regard the term in

V_{a}

in Equation (151) satisfies Equation (145) is the second-kind gauge degree of freedom and we regard this degree of freedom as an “unphysical degree of freedom.” As in the case of the

l = 1

odd-mode perturbations, we introduce the indicator function

R_{(e)} [*]

\begin{matrix} R_{(e)} [ζ_{(e) h}] : = - \frac{1}{f} \partial_{t}^{2} ζ_{(e) h} + \partial_{r} (f \partial_{r} ζ_{(e) h}) - \frac{1 - f}{r^{2}} ζ_{(e) h} . \end{matrix}

(155)

R_{(e)} [ζ_{(e)}] = 0

, we should regard

ζ_{(e)}

is the second-kind gauge degree of freedom and we regard

ζ_{(e)}

as an “unphysical degree of freedom.”

To clarify the second-kind gauge degree of freedom, we consider the gauge-transformation rule of the tensor field

H_{a b}

through the gauge-transformation rules (132) and (134) as

\begin{matrix} {}_{Y}H_{a b} - {}_{X}H_{a b} \\ : = & ({}_{Y} H_{A B} - {}_{X} H_{A B}) cos θ {(d x^{A})}_{(a} {(d x^{B})}_{b)} + \frac{r^{2}}{2} ({}_{Y} H - {}_{X} H) cos θ γ_{a b} \end{matrix}

\begin{matrix} = & - 2 r [\partial_{t}^{2} ζ_{(e) h} - \frac{f (1 - f)}{2 r} \partial_{r} ζ_{(e) h} + \frac{f (1 - f)}{2 r^{2}} ζ_{(e) h}] cos θ {(d t)}_{a} {(d t)}_{b} \\ - 4 r [\partial_{t} \partial_{r} ζ_{(e) h} - \frac{1 - f}{2 r f} \partial_{t} ζ_{(e) h}] cos θ {(d t)}_{(a} {(d r)}_{b)} \\ - 2 r [\partial_{r}^{2} ζ_{(e) h} + \frac{1 - f}{2 r f} \partial_{r} ζ_{(e) h} - \frac{1 - f}{2 r^{2} f} ζ_{(e) h}] cos θ {(d r)}_{a} {(d r)}_{b} \end{matrix}

\begin{matrix} - 2 r^{2} (f \partial_{r} ζ_{(e) h} + \frac{1}{r} (1 - f) ζ_{(e) h}) cos θ γ_{a b} \end{matrix}

(156)

\begin{matrix} = & £_{W} g_{a b}, \end{matrix}

(157)

where

\begin{matrix} W_{a} & = & - r \partial_{t} ζ_{(e) h} cos θ {(d t)}_{a} + (ζ_{(e) h} - r \partial_{r} ζ_{(e) h}) cos θ {(d r)}_{a} - r ζ_{(e) h} sin θ {(d θ)}_{a} . \end{matrix}

(158)

Comparing Equation (157) with the generator (158) and Equation (151) with the generator (152), there is the possibility that the Lie derivative term

£_{V} g_{a b}

in the solution (151) is “residual gauge degree of freedom” with the identification

\begin{matrix} Φ_{(e)} = ζ_{(e) h} . \end{matrix}

(159)

For this reason, we check the indicator (155). From Equation (153), we obtain

\begin{matrix} R_{(e)} [Φ_{(e)}] : = \frac{16 π r}{3 (1 - f)} S_{(Φ_{(e)})} . \end{matrix}

(160)

Therefore, the variable

Φ_{(e)}

should be regarded as the second-kind gauge degree of freedom and is the “unphysical degree of freedom” if

S_{(Φ_{(e)})} = 0

, while in the non-vacuum case

S_{Φ_{(e)}} \neq 0

, the indicator (160) yields

R_{(e)} [Φ_{(e)}] \neq 0

. This means that

Φ_{(e)}

is not the second-kind gauge degree of freedom but is the “physical degree of freedom” in the non-vacuum case

S_{Φ_{(e)}} \neq 0

. Due to this existence of the source term, the identification (160) is impossible in the case of the non-vacuum situation. Rather, this term is gauge-invariant in the sense of the second kind, and we regard this term as a gauge-degree of freedom of the first kind in the non-vacuum case.

Although we have

R_{(e)} [Φ_{(e)}] = 0

in the case where

S_{Φ_{(e)}} = 0

and we should regard

Φ_{(e)}

is a “gauge degree of freedom of the second kind”, Equation (161) indicates that

\begin{matrix} R_{(e)} [Φ_{(e)}] = - \frac{1}{f} \partial_{t}^{2} Φ_{(e)} + \partial_{r} (f \partial_{r} Φ_{(e)}) - \frac{1 - f}{r^{2}} Φ_{(e)} = 0 . \end{matrix}

(161)

This coincides with the left-hand side of Equation (153). Therefore, as in the case of the

l = 1

odd-mode perturbations, we consider the following two sets of function

Φ_{(e)}

\begin{matrix} G_{(e)} & : = & \{Φ_{(e)}| R_{(o)} [Φ_{(e)}] = 0\}, \end{matrix}

(162)

\begin{matrix} H_{(e)} & : = & \{Φ_{(e)}| - \frac{1}{f} \partial_{t}^{2} Φ_{(e)} + \partial_{r} (f \partial_{r} Φ_{(e)}) - \frac{1 - f}{r^{2}} Φ_{(e)} = 0\} . \end{matrix}

(163)

From Equation (161), we obtain the relation

\begin{matrix} G_{(e)} = H_{(e)} . \end{matrix}

(164)

This indicates that any homogeneous solution (without source term) to Equation (153) should be regarded as a gauge degree of freedom of the second kind which is the “unphysical degree of freedom.”

On the other hand, to obtain the explicit solution

Φ_{(e)}

in the case

S_{Φ_{(e)}} \neq 0

, which is regarded as a “physical degree of freedom,” we have to solve Equation (153) with appropriate boundary conditions. Equation (153) is an inhomogeneous second-order linear differential equation for

Φ_{(e)}

and its boundary conditions are adjusted by the homogeneous solutions to Equation (153), i.e., the element of the set of function

H_{(e)}

. However, any homogeneous solution to Equation (153) should be regarded as an “unphysical degree of freedom” in the “complete gauge fixing approach” as mentioned above. Therefore, in the conventional “complete gauge fixing approach”, we have to impose the boundary conditions for Equation (118) using a homogeneous solution, which is regarded as an “unphysical degree of freedom,” to obtain a “physical solution” to Equation (118) with nonvanishing source term

S_{Φ_{(e)}} \neq 0

. This situation is a dilemma. In this sense, as in the case of

l = 1

odd-mode perturbations, a conventional “complete gauge-fixing approach” includes a stronger restriction than our proposed gauge-invariant formulation.

6. l=0 Mode Perturbation in the Conventional Approach

6.1. Einstein Equations for $l = 0$ Mode Perturbations

Here, we consider the

l = 0

mode perturbations which are described by Equations (94)–(96). Substitution of Equations (94)–(96) into Equations (A16)–(A18), we obtain the

l = 0

mode perturbations of the linearized Einstein tensor. We use the background Einstein equations (Equation (B67) and (B68) of Appendix B in the Part I paper [14]). Then, we obtain the non-trivial components of the

l = 0

mode Einstein equation

{}^{(1)} G_{a}^{b} = 8 π {}^{(1)} T_{a}^{b}

are given by

\begin{matrix} - \frac{1}{2} {\bar{D}}_{C} {\bar{D}}^{C} {\tilde{h}}_{A}^{B} + \frac{1}{2} {\bar{D}}^{B} {\bar{D}}^{C} {\tilde{h}}_{A C} + \frac{1}{2} {\bar{D}}_{A} {\bar{D}}_{C} {\tilde{h}}^{B C} - \frac{1}{2} {\bar{D}}_{A} {\bar{D}}^{B} {\tilde{h}}_{C}^{C} \\ - \frac{1}{r} ({\bar{D}}^{C} r) {\bar{D}}_{C} {\tilde{h}}_{A}^{B} + \frac{1}{r} ({\bar{D}}^{C} r) {\bar{D}}^{B} {\tilde{h}}_{A C} + \frac{1}{r} ({\bar{D}}_{C} r) {\bar{D}}_{A} {\tilde{h}}^{B C} - \frac{2}{r^{2}} ({\bar{D}}^{C} r) ({\bar{D}}_{C} r) {\tilde{h}}_{A}^{B} \\ - \frac{1}{2 r} ({\bar{D}}^{B} r) {\bar{D}}_{A} {\tilde{h}}_{(e 0)} - \frac{1}{2 r} ({\bar{D}}_{A} r) {\bar{D}}^{B} {\tilde{h}}_{(e 0)} - \frac{1}{2} {\bar{D}}_{A} {\bar{D}}^{B} {\tilde{h}}_{(e 0)} + \frac{2}{r^{2}} {\tilde{h}}_{A}^{B} \\ + y_{A}^{B} (- \frac{1}{2} {\bar{D}}_{C} {\bar{D}}_{D} {\tilde{h}}^{C D} + \frac{1}{2} {\bar{D}}_{C} {\bar{D}}^{C} {\tilde{h}}_{D}^{D} - \frac{2}{r} ({\bar{D}}_{D} r) {\bar{D}}_{C} {\tilde{h}}^{C D} + \frac{1}{r} ({\bar{D}}^{C} r) {\bar{D}}_{C} {\tilde{h}}_{D}^{D} \\ - \frac{1}{r^{2}} ({\bar{D}}_{C} r) ({\bar{D}}_{D} r) {\tilde{h}}^{C D} + \frac{3}{2 r^{2}} ({\bar{D}}^{D} r) ({\bar{D}}_{D} r) {\tilde{h}}_{C}^{C} - \frac{3}{2 r^{2}} {\tilde{h}}_{C}^{C} \\ + \frac{1}{2 r^{2}} {\tilde{h}}_{(e 0)} + \frac{3}{2 r} ({\bar{D}}^{C} r) {\bar{D}}_{C} {\tilde{h}}_{(e 0)} + \frac{1}{2} {\bar{D}}_{C} {\bar{D}}^{C} {\tilde{h}}_{(e 0)}) \end{matrix}

(165)

\begin{matrix} = & 8 π {\tilde{T}}_{A}^{B}, \\ {\bar{D}}_{C} {\bar{D}}^{C} {\tilde{h}}_{D}^{D} - {\bar{D}}_{C} {\bar{D}}_{D} {\tilde{h}}^{C D} - \frac{2}{r} ({\bar{D}}_{C} r) {\bar{D}}_{D} {\tilde{h}}^{C D} + \frac{1}{r} ({\bar{D}}^{C} r) {\bar{D}}_{C} {\tilde{h}}_{D}^{D} \\ + \frac{1}{2} {\bar{D}}_{C} {\bar{D}}^{C} {\tilde{h}}_{(e 0)} + \frac{1}{r} ({\bar{D}}^{C} r) {\bar{D}}_{C} {\tilde{h}}_{(e 0)} \end{matrix}

\begin{matrix} = & 8 π {\tilde{T}}_{(e 0)} . \end{matrix}

(166)

Here, we decomposition of the component

{\tilde{h}}_{A B}

\begin{matrix} {\tilde{h}}_{A B} = : {\tilde{H}}_{A B} + \frac{1}{2} y_{A B} {\tilde{h}}_{C}^{C} . \end{matrix}

(167)

In terms of the variables defined by Equation (169), the linearization of the Einstein equations for

l = 0

mode are summarized as follows. The trace of

{}^{(1)} G_{A}^{B} = 8 π {}^{(1)} T_{A}^{B}

for

l = 0

mode is given by

\begin{matrix} - \frac{1}{r^{2}} {\tilde{h}}_{C}^{C} - \frac{2}{r} ({\bar{D}}_{C} r) (+ {\bar{D}}_{D} {\tilde{H}}^{D C} + \frac{1}{r} ({\bar{D}}_{D} r) {\tilde{H}}^{C D}) \\ + \frac{1}{2} {\bar{D}}_{C} {\bar{D}}^{C} {\tilde{h}}_{(e 0)} + \frac{2}{r} ({\bar{D}}_{C} r) {\bar{D}}^{C} {\tilde{h}}_{(e 0)} + \frac{1}{r^{2}} {\tilde{h}}_{(e 0)} = 8 π {\tilde{T}}_{C}^{C} . \end{matrix}

(168)

The traceless part of

{}^{(1)} G_{A}^{B} = 8 π {}^{(1)} T_{A}^{B}

for

l = 0

mode is given by

\begin{matrix} - \frac{1}{2} [{\bar{D}}_{C} {\bar{D}}^{C} + \frac{2}{r} ({\bar{D}}^{C} r) {\bar{D}}_{C} + \frac{4}{r^{2}} ({\bar{D}}^{C} r) ({\bar{D}}_{C} r) - \frac{4}{r^{2}}] {\tilde{H}}_{A B} \\ + {\bar{D}}_{(A} {\bar{D}}^{C} {\tilde{H}}_{B) C} - \frac{1}{2} y_{A B} {\bar{D}}_{C} {\bar{D}}_{D} {\tilde{H}}^{C D} + \frac{2}{r} ({\bar{D}}^{C} r) ({\bar{D}}_{(A} {\tilde{H}}_{B) C} - \frac{1}{2} y_{A B} {\bar{D}}^{D} {\tilde{H}}_{D C}) \\ + \frac{1}{r} (({\bar{D}}_{(A} r) {\bar{D}}_{B)} {\tilde{h}}_{E}^{E} - \frac{1}{2} y_{A B} ({\bar{D}}^{C} r) {\bar{D}}_{C} {\tilde{h}}_{D}^{D}) - \frac{1}{2} [{\bar{D}}_{A} {\bar{D}}_{B} {\tilde{h}}_{(e 0)} - \frac{1}{2} y_{A B} {\bar{D}}_{C} {\bar{D}}^{C} {\tilde{h}}_{(e 0)}] \\ - \frac{1}{r} [({\bar{D}}_{(A} r) {\bar{D}}_{B)} {\tilde{h}}_{(e 0)} - \frac{1}{2} y_{A B} ({\bar{D}}^{C} r) {\bar{D}}_{C} {\tilde{h}}_{(e 0)}] = 8 π [{\tilde{T}}_{A B} - \frac{1}{2} y_{A B} {\tilde{T}}_{C}^{C}] . \end{matrix}

(169)

Furthermore,

{}^{(1)} G_{p}^{q} = 8 π {}^{(1)} T_{p}^{q}

for

l = 0

mode is given by

\begin{matrix} \frac{1}{2} {\bar{D}}_{C} {\bar{D}}^{C} {\tilde{h}}_{(e 0)} + \frac{1}{r} ({\bar{D}}^{C} r) {\bar{D}}_{C} {\tilde{h}}_{(e 0)} - {\bar{D}}_{C} {\bar{D}}_{D} {\tilde{H}}^{C D} - \frac{2}{r} ({\bar{D}}_{C} r) {\bar{D}}_{D} {\tilde{H}}^{C D} + \frac{1}{2} {\bar{D}}_{C} {\bar{D}}^{C} {\tilde{h}}_{D}^{D} \\ = & 8 π {\tilde{T}}_{(e 0)} . \end{matrix}

(170)

6.2. Gauge-Fixing for $l = 0$ Mode Perturbations

We consider the gauge-transformation rules (97) and (98) of the mode coefficient

{\tilde{h}}_{A B}

and

{\tilde{h}}_{(e 0)}

. If these gauge-transformation rules are those of the second kind, we should exclude these gauge degrees of freedom through some gauge-fixing procedure, because the degree of freedom of the second-kind gauge is the unphysical degree of freedom.

In the static chart in which the metric

y_{A B}

is given by Equation (17). Through the static chart (17), the gauge-transformation rule (98) is given by

\begin{matrix} {}_{Y} {\tilde{h}}_{(e 0)} - {}_{X} {\tilde{h}}_{(e 0)} = \frac{4}{r} f ζ_{r} . \end{matrix}

(171)

Then we may choose

ζ_{r}

so that

\begin{matrix} {}_{Y} {\tilde{h}}_{(e 0)} & = & {}_{X} {\tilde{h}}_{(e 0)} + \frac{4}{r} f ζ_{r} = 0, \end{matrix}

(172)

i.e.,

\begin{matrix} ζ_{r} = - \frac{r}{4 f} {}_{X} {\tilde{h}}_{(e 0)} . \end{matrix}

(173)

Through this gauge-fixing, we may regard

{\tilde{h}}_{(e 0)} = 0

in the

Y

-gauge.

As the gauge-fixing for

{\tilde{h}}_{A B}

, we fix the gauge so that

{\tilde{h}}_{A B}

is traceless. This gauge-fixing so that

{\tilde{h}}_{A B}

is traceless makes easy to compare with our gauge-invariant expression in Refs. [12,13,14,15,16]. The trace of the gauge transformation rue Equation (97), we obtain

\begin{matrix} y^{A B} {}_{Y} {\tilde{h}}_{A B} - y^{A B} {}_{X} {\tilde{h}}_{A B} & = & {}_{Y} {\tilde{h}}_{C}^{C} - {}_{X} {\tilde{h}}_{C}^{C} = 2 {\bar{D}}^{C} ζ_{C} . \end{matrix}

(174)

In the static chart (17) of the Schwarzschild spacetime, the gauge transformation rule (174) is given by

\begin{matrix} {}_{Y} {\tilde{h}}_{C}^{C} - {}_{X} {\tilde{h}}_{C}^{C} & = & - 2 f^{- 1} \partial_{t} ζ_{t} + 2 \partial_{r} (f ζ_{r}) . \end{matrix}

(175)

From this gauge-transformation rule and the gauge fixing (173), we may fix the gauge degree of freedom

ζ_{t}

so that

\begin{matrix} 0 & = & {}_{Y} {\tilde{h}}_{C}^{C} \\ = & {}_{X} {\tilde{h}}_{C}^{C} - 2 f^{- 1} \partial_{t} ζ_{t} + 2 \partial_{r} (- \frac{r}{4} {}_{X} {\tilde{h}}_{(e 0)}) . \end{matrix}

(176)

Through this gauge-fixing, we may regard

{\tilde{h}}_{C}^{C} = 0

. However, we have to emphasize that the degree of freedom of the choice of the generator

ζ_{t}

remains the degree of freedom of an arbitrary function of r.

Thus, through the gauge-fixing (173) and (176), we may regard

\begin{matrix} {\tilde{h}}_{(e 0)} = {\tilde{h}}_{C}^{C} = 0 \end{matrix}

(177)

Under the gauge-fixing condition (177) linearization of the Einstein equations for

l = 0

mode are summarized as

\begin{matrix} - ({\bar{D}}_{C} r) {\bar{D}}_{D} {\tilde{H}}^{D C} - \frac{1}{r} ({\bar{D}}_{C} r) ({\bar{D}}_{D} r) {\tilde{H}}^{C D} = 4 π r {\tilde{T}}_{C}^{C}, \end{matrix}

(178)

\begin{matrix} - \frac{1}{2} [{\bar{D}}_{C} {\bar{D}}^{C} + \frac{2}{r} ({\bar{D}}^{C} r) {\bar{D}}_{C} + \frac{4}{r^{2}} ({\bar{D}}^{C} r) ({\bar{D}}_{C} r) - \frac{4}{r^{2}}] {\tilde{H}}_{A B} + {\bar{D}}_{(A} {\bar{D}}^{C} {\tilde{H}}_{B) C} \\ - \frac{1}{2} y_{A B} {\bar{D}}_{C} {\bar{D}}_{D} {\tilde{H}}^{C D} + \frac{2}{r} ({\bar{D}}^{C} r) (+ {\bar{D}}_{(A} {\tilde{H}}_{B) C} - \frac{1}{2} y_{A B} {\bar{D}}^{D} {\tilde{H}}_{D C}) \\ = & 8 π [{\tilde{T}}_{A B} - \frac{1}{2} y_{A B} {\tilde{T}}_{C}^{C}], \end{matrix}

(179)

and

\begin{matrix} - {\bar{D}}_{C} {\bar{D}}_{D} {\tilde{H}}^{C D} - \frac{2}{r} ({\bar{D}}_{C} r) {\bar{D}}_{D} {\tilde{H}}^{C D} = 8 π {\tilde{T}}_{(e 0)} . \end{matrix}

(180)

6.3. Component Expression of the Linearized $l = 0$ Gauge-Fixed field equations

Here, we consider the component representations of Equations (178)–(180). To do this, we consider the components of the traceless tensor

{\tilde{H}}_{A B}

\begin{matrix} {\tilde{H}}_{A B} = : X_{(e)} [{(d t)}_{A} {(d t)}_{B} + f^{- 2} {(d r)}_{A} {(d r)}_{B}] + 2 Y_{(e)} {(d t)}_{(A} {(d r)}_{B)} . \end{matrix}

(181)

Here, we use the background Einstein equation (B65) of Appendix B in the Part I paper [14], i.e.,

\begin{matrix} \partial_{r} f = \frac{1 - f}{r} . \end{matrix}

(182)

Then, we obtain

\begin{matrix} \partial_{r}^{2} f = \partial_{r} (\frac{1 - f}{r}) = - \frac{2 (1 - f)}{r^{2}} \end{matrix}

(183)

Through Equations (182) and (183), Equation (178) is given by

\begin{matrix} r f \partial_{t} Y_{(e)} - r f \partial_{r} X_{(e)} - f X_{(e)} = - 4 π r^{2} ({\tilde{T}}_{t t} - f^{2} {\tilde{T}}_{r r}) . \end{matrix}

(184)

The

(A, B) = (t, t)

and

(A, B) = (r, r)

components of Equation (179) yield the same equation as

\begin{matrix} r f \partial_{t} Y_{(e)} = 4 π r^{2} ({\tilde{T}}_{t t} + f^{2} {\tilde{T}}_{r r}) . \end{matrix}

(185)

The

(A, B) = (t, r)

component of Equation (179) is given by

\begin{matrix} \partial_{t} X_{(e)} = 8 π r f {\tilde{T}}_{t r} . \end{matrix}

(186)

In terms of the components (181), Equation (180) is given by

\begin{matrix} - \partial_{t}^{2} X_{(e)} - f^{2} \partial_{r}^{2} X_{(e)} - \frac{2}{r} f^{2} \partial_{r} X_{(e)} + 2 f^{2} \partial_{t} \partial_{r} Y_{(e)} + \frac{1}{r} f (1 + f) \partial_{t} Y_{(e)} = 8 π f^{2} {\tilde{T}}_{(e 0)} . \end{matrix}

(187)

On the other hand, the even-mode perturbation of the divergence of the energy-momentum tensor is given by Equations (60) and (60). However, Equation (60) does not appear due to

{\hat{D}}_{p} S = ϵ_{p q} {\hat{D}}^{q} S = 0

. Then, the non-trivial

l = 0

components of the divergence of the energy-momentum tensor are given by

\begin{matrix} {\bar{D}}^{C} {\tilde{T}}_{C}^{B} + \frac{2}{r} ({\bar{D}}^{D} r) {\tilde{T}}_{D}^{B} - \frac{1}{r} ({\bar{D}}^{B} r) {\tilde{T}}_{(e 0)} = 0 . \end{matrix}

(188)

The

B = t

component of Equation (188) is given by

\begin{matrix} \partial_{t} {\tilde{T}}_{t t} - f^{2} \partial_{r} {\tilde{T}}_{r t} - \frac{1}{r} f (1 + f) {\tilde{T}}_{r t} = 0 . \end{matrix}

(189)

and

B = r

component of Equation (188) is given by

\begin{matrix} - f \partial_{t} {\tilde{T}}_{t r} + f^{3} \partial_{r} {\tilde{T}}_{r r} + \frac{1}{2 r} (1 - f) {\tilde{T}}_{t t} + \frac{1}{2 r} f^{2} (3 + f) {\tilde{T}}_{r r} - \frac{1}{r} f^{2} {\tilde{T}}_{(e 0)} = 0 . \end{matrix}

(190)

Substituting Equation (185) into Equation (184), we obtain

\begin{matrix} \partial_{r} (r X_{(e)}) = r \partial_{r} X_{(e)} + X_{(e)} = 8 π \frac{r^{2}}{f} {\tilde{T}}_{t t} . \end{matrix}

(191)

Substituting Equations (185), (186), and (191) into Equation (187), we obtain

\begin{matrix} 0 & = & - f \partial_{t} {\tilde{T}}_{t r} + f^{3} \partial_{r} {\tilde{T}}_{r r} + \frac{1}{2 r} (1 - f) {\tilde{T}}_{t t} + \frac{1}{2 r} f^{2} (3 + f) {\tilde{T}}_{r r} - \frac{1}{r} f^{2} {\tilde{T}}_{(e 0)} . \end{matrix}

This coincides with Equation (190) which indicates that Equation (187) does not give any new information other than Equation (190).

Here, we consider the integrability of Equation (186) and (191) as follows:

\begin{matrix} \partial_{r} (\partial_{t} (r X_{(e)})) - \partial_{t} (\partial_{r} (r X_{(e)})) & = & \partial_{r} (8 π r^{2} f {\tilde{T}}_{t r}) - \partial_{t} (8 π \frac{r^{2}}{f} {\tilde{T}}_{t t}) \\ = & - 8 π r^{2} [+ \partial_{t} {\tilde{T}}_{t t} - f^{2} \partial_{r} {\tilde{T}}_{t r} - \frac{1}{r} f (1 + f) {\tilde{T}}_{t r}] \\ = & 0 . \end{matrix}

(192)

Here, we used Equation (189) in the last equality. This means that the t-component (189) of the continuity equation guarantees the integrability of Equations (186) and (191). Then, from Equation (191), we may write the solution to Equations (186) and (191) under the integrability condition (189) as

\begin{matrix} X_{(e)} = \frac{1}{r} [2 M_{1} + 8 π \int d r \frac{r^{2}}{f} {\tilde{T}}_{t t}], \end{matrix}

(193)

where

M_{1}

is the constant of integration. This

M_{1}

corresponds to the perturbation of the Schwarzschild mass parameter.

On the other hand, in the linearized Einstein equation, there is no equation for

\partial_{r} Y_{(e)}

which guarantees the integrability condition for Equation (185). However, we may write the solution to the equation (185) as

\begin{matrix} Y_{(e)} = \frac{4 π r}{f} \int d t ({\tilde{T}}_{t t} + f^{2} {\tilde{T}}_{r r}) + Y_{(e) 0} (r) . \end{matrix}

(194)

where

Y_{(e) 0} (r)

is an arbitrary function of r. There is no equation that determines the arbitrary function

Y_{(e) 0} (r)

of r within the linearized Einstein equations.

From the definition (181) of the metric perturbation

{\tilde{H}}_{A B}

and the solutions (193) and (194), we obtain

\begin{matrix} {\tilde{H}}_{A B} & = & \frac{2}{r} (M_{1} + 4 π \int d r \frac{r^{2}}{f} {\tilde{T}}_{t t}) ({(d t)}_{A} {(d t)}_{B} + f^{- 2} {(d r)}_{A} {(d r)}_{B}) \\ 2 [4 π r \int d t (\frac{1}{f} {\tilde{T}}_{t t} + f {\tilde{T}}_{r r}) + Y_{(e) 0} (r)] {(d t)}_{(A} {(d r)}_{B)} . \end{matrix}

(195)

Here, the components of the energy-momentum tensor satisfy the continuity equations (189) and (190).

To interpret the term of

Y_{(e) 0} (r)

in Equation (195), we consider the term

£_{V} g_{a b}

with the generator

V_{a}

whose components are given by

\begin{matrix} V_{a} = V_{t} (r) {(d t)}_{a} . \end{matrix}

(196)

Then, the nonvanishing components of

£_{V} g_{a b}

are given by

\begin{matrix} £_{V} g_{t r} & = & f \partial_{r} (\frac{1}{f} V_{t}) . \end{matrix}

(197)

Choosing

V_{t}

so that

\begin{matrix} f \partial_{r} (\frac{1}{f} V_{t}) = Y_{(e) 0} (r), V_{t} = f \int d r \frac{1}{f} Y_{(e) 0} (r), \end{matrix}

(198)

we obtain

\begin{matrix} £_{V} g_{t r} & = & Y_{(e) 0} (r) . \end{matrix}

(199)

Then, the solution (195) is given by

\begin{matrix} {\tilde{H}}_{a b} & = & \frac{2}{r} (M_{1} + 4 π \int d r \frac{r^{2}}{f} {\tilde{T}}_{t t}) ({(d t)}_{a} {(d t)}_{b} + f^{- 2} {(d r)}_{a} {(d r)}_{b}) \\ + 8 π r \int d t (\frac{1}{f} {\tilde{T}}_{t t} + f {\tilde{T}}_{r r}) {(d t)}_{(a} {(d r)}_{b)} + £_{V} g_{a b}, \end{matrix}

(200)

where

\begin{matrix} V_{a} = (f \int d r \frac{1}{f} Y_{(e) 0} (r)) {(d t)}_{a} . \end{matrix}

(201)

As noted just after Equation (176), there is still the remaining degree of freedom of gauge whose generator is given by

\begin{matrix} ζ_{a} = ζ_{t} (r) d t_{a}, \end{matrix}

(202)

where

ζ_{t} (r)

is an arbitrary function of r. Therefore, we may regard the degree of freedom of

V_{a}

given in Equation (201) can be eliminated as the second-kind gauge degree of freedom (202). According to our rule of the comparison between our gauge-invariant formulation and a “conventional complete gauge-fixing approach,” we have to regard that the degree of freedom of

V_{a}

given in Equation (201) is “unphysical.”

Thus, as the “physical solution” for

l = 0

-mode linearized Einstein equation based of a “conventional complete gauge-fixing approach,” we obtain

\begin{matrix} h_{a b} & = & \frac{2}{r} (M_{1} + 4 π \int d r \frac{r^{2}}{f} {\tilde{T}}_{t t}) ({(d t)}_{a} {(d t)}_{b} + f^{- 2} {(d r)}_{a} {(d r)}_{b}) \\ + 8 π r \int d t (\frac{1}{f} {\tilde{T}}_{t t} + f {\tilde{T}}_{r r}) {(d t)}_{(a} {(d r)}_{b)} . \end{matrix}

(203)

This coincides with the solution obtained in Refs. [12,15] except for the terms of the Lie derivative of the background metric

g_{a b}

. Therefore, we conclude that the

l = 0

solution except for the terms of the Lie derivative of the background metric

g_{a b}

obtained in Refs. [12,15] can be also obtained as (203) through a complete gauge-fixing approach.

The difference between our solution in Refs. [12,15] is in the term of the Lie derivative of the background metric. As shown above, according to our rule of comparison between our gauge-invariant formulation and a “conventional complete gauge-fixing approach,” all terms of the Lie derivative of the background metric should be regarded as the second-kind gauge degree of freedom, and these are “unphysical degree of freedom” in the above solution (203). On the other hand, in our gauge-invariant formulation developed in Refs. [12,13,14,15,16],

l = 0, 1

-mode metric perturbations are given in a gauge-invariant form and the terms of the Lie derivative of the background metric is included in these gauge-invariant variables. Since the second-kind gauge degree of freedom is completely excluded in our gauge-invariant formulation, we cannot regard these terms of the Lie derivative of the background metric as an “unphysical degree of freedom.” Therefore, we regard the terms of the Lie derivative of the background metric in these gauge-invariant variables as first-kind gauges that have some physical meaning. This point is the essential difference of the solutions in Refs. [12,13,14,15,16] and the above solutions based on a “conventional complete gauge-fixing approach.” This difference leads to the confusion of the interpretation of the perturbative Tolman Bondi solution, as shown in the next subsection.

6.4. Comparing with Lemaître-Olman-Bondi Solution

6.4.1. Perturbative expression of the LTB solution on Schwarzschild background spacetime

Here, we consider the Lemaître-Tolman-Bondi (LTB) solution [48] which is an exact solution to the Einstein equation with the matter field

\begin{matrix} T_{a b} = ρ u_{a} u_{b}, u_{a} = - {(d τ)}_{a}, \end{matrix}

(204)

and the metric

\begin{matrix} g_{a b} & = & - {(d τ)}_{a} {(d τ)}_{b} + \frac{{(\partial_{R} r)}^{2}}{1 + f (R)} {(d R)}_{a} {(d R)}_{b} + r^{2} γ_{a b}, r = r (τ, R) . \end{matrix}

(205)

This solution is a spherically symmetric solution to the Einstein equation. The function

r = r (τ, R)

satisfies the differential equation

\begin{matrix} {(\partial_{τ} r)}^{2} = \frac{F (R)}{r} + f (R) . \end{matrix}

(206)

Here, we note that

F (R)

is an arbitrary function of R representing the dust matter’s initial distribution.

f (R)

is also an arbitrary function of R that represents the initial distribution of the energy of the dust field in the Newtonian sense. The solution to Equation (206) is given in the three cases

(i): $f (R) > 0$ :

\begin{matrix} r = \frac{F (R)}{2 f (R)} (cosh η - 1), τ_{0} (R) - τ = \frac{F (R)}{2 f {(R)}^{3 / 2}} (sinh η - η), \end{matrix}

(207)

(ii): $f (R) < 0$ :

\begin{matrix} r = \frac{F (R)}{- 2 f (R)} (1 - cos η), τ_{0} (R) - τ = \frac{F (R)}{2 {(- f (R))}^{3 / 2}} (η - sin η), \end{matrix}

(208)

(iii): $f (R) = 0$ :

\begin{matrix} r = {(\frac{9 F (R)}{4})}^{1 / 3} {[τ_{0} (R) - τ]}^{2 / 3} . \end{matrix}

(209)

The energy density

ρ

is given by

\begin{matrix} 8 π ρ = \frac{\partial_{R} F}{(\partial_{R} r) r^{2}} . \end{matrix}

(210)

The LTB solution includes the three arbitrary functions

f (R)

F (R)

, and

τ_{0} (R)

Here, we consider the vacuum case

ρ = 0

. In this case, from Equation (210), we have

\begin{matrix} \partial_{R} F = 0, F = 2 M, \end{matrix}

(211)

where M is the Schwarzschild metric with the mass parameter M. Furthermore, we consider the case

f (R) = 0

. Here, we chose

τ_{0} = R

, i.e.,

\partial_{R} τ_{0} = 1

. In this case, Equation (209) yields

\begin{matrix} {(d R)}_{a} & = & {(d τ)}_{a} + {(\frac{2 M}{r})}^{- 1 / 2} {(d r)}_{a} . \end{matrix}

(212)

Then, the metric (205) is given by

\begin{matrix} g_{a b} & = & - {(d τ)}_{a} {(d τ)}_{b} + {(\partial_{R} r)}^{2} {(d R)}_{a} {(d R)}_{b} + r^{2} γ_{a b} \\ = & - f {(d t)}_{a} {(d t)}_{b} + f^{- 1} {(d r)}_{a} {(d r)}_{b} + r^{2} γ_{a b}, f = 1 - \frac{2 M}{r}, \end{matrix}

(213)

where

{(d t)}_{a}

is defined by

\begin{matrix} {(d t)}_{a} : = {(d τ)}_{a} - f^{- 1} {(1 - f)}^{1 / 2} {(d r)}_{a} . \end{matrix}

(214)

We also note that the degree of freedom of the choice of the coordinate R is completely fixed through the choice

τ_{0} = R

, though there remains a degree of freedom of the choice of

R = R (\tilde{R})

in the exact solution (205).

Now, we consider the perturbation of the Schwarzschild spacetime which is derived by the exact LTB solution (205) so that

\begin{matrix} F (R) & = & 2 [M + ϵ m_{1} (R)] + O (ϵ^{2}), \end{matrix}

(215)

\begin{matrix} f (R) & = & 0 + ϵ f_{1} (R) + O (ϵ^{2}), \end{matrix}

(216)

\begin{matrix} τ_{0} (R) & = & R + ϵ τ_{1} (R) + O (ϵ^{2}) . \end{matrix}

(217)

Through these perturbations (215)–(217), we consider the perturbative expansion of the function r which is determined by Equation (206):

\begin{matrix} r (τ, R) = r_{s} (τ, R) + ϵ r_{1} (τ, R) + O (ϵ^{2}) . \end{matrix}

(218)

Here, the function

r_{s} (τ, R)

is given by Equation (209), i.e.,

\begin{matrix} r_{s} (τ, R) = r (τ, R) = {(\frac{9 M}{2})}^{1 / 3} {[R - τ]}^{2 / 3} . \end{matrix}

(219)

In Equations (217) and (219), we chose the background value of the function

τ_{0} (R)

to be R.

Through this perturbative expansion, we evaluate

O (ϵ^{1})

perturbation of Equation (206) through Equation (212) as

\begin{matrix} {(1 - f)}^{1 / 2} (\partial_{τ} r_{1}) + \frac{m_{1} (R)}{r} - \frac{M}{r^{2}} r_{1} + \frac{1}{2} f_{1} (R) = 0, \end{matrix}

(220)

where we used Equation (212) and the replacement

r_{s} \to r

. The solution to Equation (222) is given by

\begin{matrix} r_{1} & = & {(\frac{M}{6})}^{1 / 3} \frac{m_{1} (R)}{M} {[R - τ]}^{2 / 3} - \frac{3}{20} {(\frac{6}{M})}^{1 / 3} f_{1} (R) {[R - τ]}^{+ 4 / 3} \\ + B (R) {[R - τ]}^{- 1 / 3} . \end{matrix}

(221)

From the comparison with Equation (219),

B (R)

is the perturbation of the

τ_{1} (R)

τ_{0} (R) = R + τ_{1} (R)

in the exact solution (207)–(209). Furthermore, the solution (221) can be also derived from the exact solution (207)–(209). From Equation (210), the perturbative dust energy density given by

\begin{matrix} 8 π ρ = \frac{2 \partial_{R} m_{1} (R)}{(\partial_{R} r) r^{2}} . \end{matrix}

(222)

Through the perturbative solution (221), the metric (205) is given by

\begin{matrix} g_{a b} & = & - {(d τ)}_{a} {(d τ)}_{b} + {(\partial_{R} r)}^{2} {(d R)}_{a} {(d R)}_{b} + r^{2} γ_{a b} \\ + ϵ [(2 (\partial_{R} r_{1}) - f_{1} (\partial_{R} r)) (\partial_{R} r) {(d R)}_{a} {(d R)}_{b} + 2 r r_{1} γ_{a b}] + O (ϵ^{2}) \\ = : & g_{a b}^{(0)} + ϵ {}_{X} h_{a b} + O (ϵ^{2}) . \end{matrix}

(223)

As shown in Equation (213), the background metric

g_{a b}^{(0)}

is given by the Schwarzschild metric in the static chart. On the other hand, the linear order perturbation

{}_{X} h_{a b}

(in the gauge

X_{ϵ}

) is given by

\begin{matrix} {}_{X} h_{a b} : = (2 (\partial_{R} r_{1}) - f_{1} (R) (\partial_{R} r)) (\partial_{R} r) {(d R)}_{a} {(d R)}_{b} + 2 r r_{1} γ_{a b} . \end{matrix}

(224)

Here, we fixed the second-kind gauge so that

\begin{matrix} X_{ϵ} : (τ, R, θ, ϕ) \in M_{p h} \mapsto (τ, R, θ, ϕ) \in M . \end{matrix}

(225)

Through this second-kind gauge choice and the choice of the background radial coordinate R in Equation (213), the degree of freedom of the choice of the radial coordinate

R = R (\tilde{R})

is also completely fixed even in the linearized version of the exact solution (224), which though there remains a degree of freedom of the choice of

R = R (\tilde{R})

in the exact solution (205).

Of course, if we employ the different gauge choice

Y_{ϵ}

from the above gauge-choice

X_{ϵ}

, we obtain the different expression of the metric perturbation

{}_{Y} h_{a b}

. Actually, we may choose

Y_{ϵ}

as the identification of

\begin{matrix} Y_{ϵ} : (τ + ϵ ξ^{τ} (τ, R), R + ϵ ξ^{R} (τ, R), θ, ϕ) \in M_{p h} \mapsto (τ, R, θ, ϕ) \in M . \end{matrix}

(226)

In this identification, the metric on

M_{p h}

pulled back to

M

is given by

\begin{matrix} {}_{Y_{ϵ}}g_{a b} & = & {}_{X_{ϵ}}g_{a b} + ϵ £_{ξ} g_{a b}^{(0)} + O (ϵ^{2}) \\ = & g_{a b}^{(0)} + ϵ ({}_{X} h_{a b} + £_{ξ} g_{a b}^{(0)}) + O (ϵ^{2}), \end{matrix}

(227)

where

ξ^{a} = ξ^{τ} {(\partial_{τ})}^{a} + ξ^{R} {(\partial_{R})}^{a}

is the generator of second-kind gauge transformation

X_{ϵ} \to Y_{ϵ}

6.4.2. Expression of the Perturbative LTB Solution in Static Chart

Here, we consider the expression of the linear perturbation

{}_{X} h_{a b}

given by Equation (224). From Equations (212) and (214) with

F = 2 M

, we obtain

\begin{matrix} {(d R)}_{a} & = & {(d t)}_{a} + f^{- 1} {(1 - f)}^{- 1 / 2} {(d r)}_{a}, f = 1 - \frac{2 M}{r}, \end{matrix}

(238)

\begin{matrix} {(d τ)}_{a} & = & {(d t)}_{a} + f^{- 1} {(1 - f)}^{1 / 2} {(d r)}_{a} . \end{matrix}

(229)

First, we consider the perturbation of the energy-momentum tensor of the matter field. In the case of the LTB solution, the matter field is characterized by the dust field whose energy-momentum tensor (204) is given by

\begin{matrix} T_{a b} = ρ u_{a} u_{b}, u_{a} = - {(d τ)}_{a}, u^{a} = {(\partial_{τ})}^{a} . \end{matrix}

(230)

In our case, the linearized Einstein equation gives Equation (222), i.e.,

\begin{matrix} 8 π ρ = \frac{2 \partial_{R} m_{1} (R)}{(\partial_{R} r) r^{2}} = \frac{\partial_{R} m_{1} (R)}{4 π r^{2}} {(1 - f)}^{- 1 / 2} . \end{matrix}

(231)

On the other hand, substituting Equation (229) into Equation (230), we obtain

\begin{matrix} T_{a b} & = & ρ {(d τ)}_{a} {(d τ)}_{b} \\ = & ρ ({(d t)}_{a} + f^{- 1} {(1 - f)}^{1 / 2} {(d r)}_{a}) ({(d t)}_{b} + f^{- 1} {(1 - f)}^{1 / 2} {(d r)}_{b}) \\ = & ρ {(d t)}_{a} {(d t)}_{b} + ρ \frac{{(1 - f)}^{1 / 2}}{f} 2 {(d t)}_{(a} {(d r)}_{b)} + ρ \frac{1 - f}{f^{2}} {(d r)}_{a} {(d r)}_{b} . \end{matrix}

(232)

Then, we obtain the components of the energy-momentum tensor for the static coordinate

(t, r)

\begin{matrix} {\tilde{T}}_{t t} = ρ, {\tilde{T}}_{t r} = \frac{{(1 - f)}^{1 / 2}}{f} ρ, {\tilde{T}}_{r r} = \frac{1 - f}{f^{2}} ρ, {\tilde{T}}_{(e 0)} = 0 . \end{matrix}

(233)

From this component, we can confirm the continuity equations (189) and (190).

As derived in Ref. [16], the linearized Tolman-Bondi solution (224) with the Schwarzschild background is given by

\begin{matrix} {}_{X} h_{a b} & = & \frac{2 m_{1} (R)}{r} [{(d t)}_{a} {(d t)}_{b} + \frac{1}{f^{2}} {(d r)}_{a} {(d r)}_{b}] + \frac{2 - f}{f {(1 - f)}^{1 / 2}} \frac{m_{1} (R)}{r} 2 {(d t)}_{(a} {(d r)}_{b)} \\ + £_{V_{(L T B)}} g_{a b}, \end{matrix}

(234)

where

V_{(L T B) a}

are given by

\begin{matrix} V_{(L T B) a} : = [{(1 - f)}^{1 / 2} r_{1} + \frac{1}{2} f \int d t f_{1} (R)] {(d t)}_{a} + \frac{r_{1}}{f} {(d r)}_{a} . \end{matrix}

(235)

As shown in Ref. [16], the

l = 0

solution (203) with the components (230) of the linearized energy-momentum tensor realize the first line of Equation (234). In this sense, the solutions (203) of the

l = 0

mode perturbations are justified by the LTB solutions.

However, we emphasize that the linearized LTB solution (234) does have the term

£_{V_{L T B}} g_{a b}

. As noted by Equations (228) and (229), we can always eliminate the terms of the Lie derivative of the background metric as the second-kind gauge-degree of freedom. Therefore, according to our rule of the comparison, the term

£_{V_{(L T B)}} g_{a b}

should be regarded as the second-kind gauge-degree of freedom in the “conventional gauge-fixing approach” discussed in this paper. In this case, we have to regard that the perturbation

f_{1} (R)

of the initial distribution

f (R)

of the energy of dust field in Equation (206) is an “unphysical degree of freedom” in spite that the behavior of the LTB solution crucially depends on the signature of the function

f (R)

as shown in Equations (207)–(209).

7. Summary and Discussions

In this paper, we have discussed comparison of our gauge-invariant formulation for

l = 0, 1

perturbations on the Schwarzschild background spacetime proposed in the series of papers [12,13,14,15,16] and a “conventional complete gauge-fixing approach.” It is well-known that we cannot construct gauge-invariant variables for

l = 0, 1

mode perturbations through a similar manner to the construction of the gauge-invariant variables for

l \geq 2

mode perturbations if we use the decomposition formula (26)–(28) with the spherical harmonic functions

Y_{l m}

as the scalar harmonics

S_{δ}

. In our gauge-invariant formulation for

l = 0, 1

perturbations on the Schwarzschild background spacetime, we proposed the introduction of the singular harmonic function at once. Due to this, we can construct gauge-invariant variables for

l = 0, 1

-mode perturbations in a similar manner to the

l \geq 2

modes of perturbations. After deriving the mode-by-mode perturbative Einstein equations in terms of the gauge-invariant variables, we impose the regularity on the introduced singular harmonics when we solve the derived Einstein equations. Based on this proposal, we derived formal solutions to the

l = 0, 1

-mode linearized Einstein equations without the specification of the components of the linear perturbation of the energy-momentum tensor [12,14,15]. Our proposal enables us to develop higher-order perturbations of the Schwarzschild spacetime [13]. Furthermore, we check that our derived solutions realized the linearized version of the LTB solution and non-rotating C-metric [15]. In this sense, we conclude that our proposal is physically reasonable. On the other hand, it is often said that “gauge-invariant formulations in general-relativistic perturbations are equivalent to complete gauge-fixing approaches.” For this reason, we check this statement through the comparison of our gauge-invariant formulation and a “conventional complete gauge-fixing approach” in which we use the spherical harmonic functions

Y_{l m}

as the scalar harmonics

S_{δ}

from the starting point.

After reviewing the concept of “gauges” in general relativistic perturbation theories and our proposed gauge-invariant formulation for the

l = 0, 1

-mode perturbations and our derived

l = 0, 1

-mode solutions, we considered

l = 1

odd-mode perturbations,

l = 1

even-mode perturbations, and

l = 0

even-mode perturbations, separately. As a result, it is shown that we can actually derive similar solutions even in the treatment of the “conventional complete gauge-fixing approach.” However, we have to emphasize that the derived solutions are slightly different from those derived based on our gauge-invariant formulation from a conceptual point of view.

In the case of

l = 1

odd-mode perturbations, we obtained the formal solution to the linearized Einstein equation through our proposed gauge-invariant formulation. This formal solution includes the term of the Lie derivative of the background metric. In our gauge-invariant formulation, we describe the solutions only through gauge-invariant variables. Therefore, we should regard the term of the Lie derivative of the background metric is gauge invariant. On the other hand, in the conventional gauge-fixing approach where we use the spherical harmonics

Y_{l m}

from the starting point, we cannot construct gauge-invariant variable for

l = 1

odd-mode perturbations in a similar manner to those for

l \geq 2

mode perturbations. For this reason, we have to treat gauge-dependent variables for perturbations. However, the linearized Einstein equations and the continuity equations of the linearized energy-momentum tensor for

l = 1

odd-mode perturbations in terms of these gauge-dependent variables have the completely same form that is derived through our gauge-invariant formulation. Therefore, the same formal solutions derived through our gauge-invariant formulation should be the formal solutions to these linearized Einstein equations and the continuity equation of the linearized energy-momentum tensor in terms of gauge-dependent variables. As noted above, we treat gauge-dependent variables in the conventional gauge-fixing approach. Therefore, the above Lie derivative terms of the background metric may include the gauge degree of freedom of the second kind, which should be regarded as an “unphysical degree of freedom.” Checking the residual gauge degree of freedom, we conclude that the above Lie derivative terms of the background metric include the second-kind gauge degree of freedom. However, in our formal solution, there is a variable that should be obtained by solving the

l = 1

Regge-Wheeler equation. We conclude that the solution to this

l = 1

Regge-Wheeler equation is not the gauge degree of freedom of the second kind but a physical degree of freedom. Furthermore, we have to impose appropriate boundary conditions to solve this

l = 1

Regge-Wheeler equation. Since the

l = 1

Regge-Wheeler equation is an inhomogeneous linear second-order partial differential equation, the boundary conditions for an inhomogeneous linear second-order partial differential equation are adjusted by the homogeneous solutions to this linear second-order partial differential equation. According to the check of the residual gauge degree of freedom, we have to conclude that a part of homogeneous solutions to this equation is the gauge degree of freedom of the second kind. We have to eliminate this part from our consideration because this gauge degree of freedom is “unphysical.” This is the restriction of the boundary conditions of the linearized Einstein equations.

In the case of

l = 1

even-mode perturbations, the situation is worse than the

l = 1

odd-mode case. As in the

l = 1

odd-mode case, we obtained the formal solution to the linearized Einstein equation through our proposed gauge-invariant formulation. This formal solution includes the term of the Lie derivative of the background metric, which is gauge-invariant within our proposed gauge-invariant formulation. On the other hand, in the conventional gauge-fixing approach where we use the spherical harmonics

Y_{l m}

from the starting point, we cannot construct gauge-invariant variable for

l = 1

even-mode perturbations in a similar manner to those for

l \geq 2

mode perturbations. For this reason, we have to treat gauge-dependent variables for perturbations. As in the

l = 1

odd-mode case, the linearized Einstein equations and the continuity equations of the linearized energy-momentum tensor for

l = 1

even-mode perturbations in terms of these gauge-dependent variables have the completely same form that is derived through our gauge-invariant formulation. Therefore, the same formal solutions derived through our gauge-invariant formulation should be the formal solutions to these linearized Einstein equations and the continuity equation of the linearized energy-momentum tensor in terms of gauge-dependent variables. As noted above, we treat gauge-dependent variables in the conventional gauge-fixing approach as in the

l = 1

odd-mode case. Therefore, the above Lie derivative terms of the background metric may include the second-kind gauge degree of freedom, which should be regarded as an “unphysical degree of freedom.” However, in our formal solution, there is a variable that should be obtained by solving the

l = 1

Zerilli equation. We conclude that the solution to this

l = 1

Zerilli equation is not the gauge degree of freedom of the second kind but the physical degree of freedom in the non-vacuum case. Furthermore, we have to impose appropriate boundary conditions to solve this

l = 1

Zerilli equation in the non-vacuum case. Since the

l = 1

Zerilli equation is an inhomogeneous linear second-order partial differential equation. The boundary conditions for an inhomogeneous linear second-order partial differential equation are adjusted by the homogeneous solutions to this linear second-order partial differential equation. According to the check of the residual gauge degree of freedom, we have to conclude that all homogeneous solutions to this equation are the gauge degree of freedom of the second kind, i.e., all homogeneous solution to the

l = 1

Zerilli equation is “unphysical.” We have to eliminate these homogeneous solutions from our consideration because these are regarded as “unphysical.” Due to this situation, we have to say that we have to impose the boundary conditions using these “unphysical degrees of freedom” to obtain the “physical solution” through

l = 1

Zerilli equation. This is a dilemma.

In the case of

l = 0

even-mode perturbations, we obtain the complete gauge fixed solution. This solution does not include any term of the Lie derivative of the background metric. All terms of the Lie derivative of the background metric are regarded as the gauge degree of freedom of the second kind. On the other hand, the solution that is derived through our proposed gauge-invariant formulation includes the terms of the Lie derivatives of the background metric which is regarded as the first-kind gauge in our gauge-invariant formulation, i.e., these are “physical.” This difference leads a problem when we compare the derived solution with the linearized LTB solution. In the linearized LTB solution, the initial energy distribution

f_{1} (R)

of the dust field in the Newtonian sense is included in the terms of the Lie derivative of the background metric. When we realize this linearized exact solution by the solution obtained by our gauge-invariant formulation, this initial energy distribution is regarded as a physical degree of freedom. On the other hand, when we realize this linearized exact solution through the solution obtained by a conventional complete gauge-fixing approach, we have to regard this initial energy distribution of the dust field as the gauge degree of freedom of the second kind and have to regard it “unphysical.” Since the behavior of the exact LTB solution crucially depends on this initial energy distribution of the dust field, it is not natural to regard that this initial degree of freedom is unphysical.

In summary, we have to conclude that there is a case where the boundary conditions and initial conditions are restricted in the conventional complete gauge-fixing approach where we use the decomposition of the metric perturbation by the spherical harmonics

Y_{l m}

from the starting point. On the other hand, such a situation does not occur in our proposed gauge-invariant formulation. As a theory of physics, this point should be regarded as the incompleteness of the conventional complete gauge-fixing approach where we use the decomposition of the metric perturbation by the spherical harmonics

Y_{l m}

from the starting point. This is the main result of this paper.

Let us discuss why such a difference occurs between our proposed gauge-invariant formulation and a conventional complete gauge-fixed approach where we use the decomposition of the metric perturbation by the spherical harmonics

Y_{l m}

from the starting point. The aim of the introduction of the singular harmonic functions in our proposed gauge-invariant formulation is to increase the degree of freedom to clarify the distinction between the gauge degree of freedom of the second kind and the physical degree of freedom. As emphasized in Sec. 3, if we choose

S = Y_{l m}

, we have

{\hat{D}}_{p} S

ϵ_{p q} {\hat{D}}^{q} S

= 0,

({\hat{D}}_{p} {\hat{D}}_{q} - \frac{1}{2} γ_{p q} {\hat{D}}^{r} {\hat{D}}_{r}) S

2 ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} S

= 0 for

l = 0

modes and

({\hat{D}}_{p} {\hat{D}}_{q} - \frac{1}{2} γ_{p q} {\hat{D}}^{r} {\hat{D}}_{r}) S

2 ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} S

= 0 for

l = 1

modes. This is the essential reason for the fact that we cannot construct gauge-invariant variables for

l = 0, 1

mode metric perturbation in a similar manner to the derivation of gauge-invariant variables for

l \geq 2

modes. Due to these vanishing vector- or tensor-harmonics, the associated mode coefficients do not appear, and we cannot construct gauge-invariant variables for

l = 0, 1

-modes in a similar manner to the case of

l \geq 2

modes. In our series of papers [12,13,14,15,16], we regarded that this is due to the lack of the degree of freedom. For this reason, in our proposed gauge-invariant formulation, we introduced singular harmonic functions

k_{\hat{Δ}}

and

k_{\hat{Δ + 2} m}

for

l = 0

and

l = 1

modes, respectively. Owing to the introduction of these singular harmonic functions, we have

{\hat{D}}_{p} S

≠ 0 ≠

ϵ_{p q} {\hat{D}}^{q} S

and

({\hat{D}}_{p} {\hat{D}}_{q} - \frac{1}{2} γ_{p q} {\hat{D}}^{r} {\hat{D}}_{r}) S

≠ 0 ≠

2 ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} S

for

l = 0

modes and

({\hat{D}}_{p} {\hat{D}}_{q} - \frac{1}{2} γ_{p q} {\hat{D}}^{r} {\hat{D}}_{r}) S

≠ 0 ≠

2 ϵ_{r (p} {\hat{D}}_{q)} {\hat{D}}^{r} S

for

l = 1

modes. Thanks to these non-vanishing vector- or tensor-harmonics, the associated mode coefficients do appear, and we can construct gauge-invariant variables for

l = 0, 1

-modes in a similar manner to the case of

l \geq 2

modes. This leads to the development of the gauge-invariant perturbation theory for all modes [12,14,15,16] and the development of the higher-order gauge-invariant perturbations [13].

As noted in the Part I paper [14], the decomposition using the spherical harmonics

Y_{l m}

from the starting point corresponds to the imposition of the regular boundary condition on

S^{2}

on the metric perturbations from the starting point. In this sense, our introduction of the singular harmonic functions corresponds to the change of the boundary conditions on

S^{2}

. As shown in the Part I paper [14], if we introduce this change of boundary conditions on

S^{2}

, we can clearly distinguish the gauge degree of freedom of the second kind and the physical degree of freedom, i.e., we can easily construct gauge-invariant variables for

l = 0, 1

-mode perturbations. This indicates that the imposition of the boundary conditions on

S^{2}

and the construction of the gauge-invariant variables does not commute as the procedure of calculations. This is the appearance of the non-locality of

l = 0, 1

-mode perturbations as pointed out in Ref. [38]. Due to these reasons, we reached the conceptual difference between the

l = 0, 1

-mode solutions discussed in this paper. Namely, in the conventional complete gauge-fixing approach where we use the decomposition by the harmonic function

Y_{l m}

from the starting point, the degree of freedom of the metric perturbations is not sufficient so that we can distinguish the gauge degree of freedom of the second kind, i.e., “unphysical modes” and “physical modes.” In spite of this situation of the lack of degree of freedom, if we dare to carry out the “complete gauge-fixing” as the “elimination of unphysical modes,” this “complete gauge-fixing” leads to the restriction of the boundary conditions and initial conditions as shown in this paper.

On the other hand, in our proposed gauge-invariant formulation, there are no conceptual difficulties, such as the restriction of the boundary conditions and initial conditions pointed out in this paper, due to the sufficient degree of freedom of the metric perturbations. Incidentally, due to this sufficient degree of freedom of the metric perturbations through the introduction of the singular harmonic functions, our proposed gauge-invariant variables are equivalent to variables of the complete gauge-fixing within our proposed formulation in which the degree of freedom of the metric perturbations is sufficiently extended. Furthermore, we can develop higher-order perturbation theory without gauge-ambiguities if we apply our proposal and there are wide applications of the higher-order gauge-invariant perturbations on the Schwarzschild background spacetime as briefly discussed in Ref. [13]. We leave these further developments of the application of our formulation to concrete problems of perturbations on the Schwarzschild background spacetime as future works.

Funding

This research received no external funding.

Acknowledgments

The author acknowledge to Dr. Masashi Kimura for pointing out essential typos in the previous version of this manuscript.

Conflicts of Interest

The authors declare no conflicts of interest.

Abbreviations

The following abbreviations are used in this manuscript:

MDPI	Multidisciplinary Digital Publishing Institute
DOAJ	Directory of open access journals
TLA	Three letter acronym
LD	Linear dichroism

Appendix A. Linearized Einstein Tensor

In this Appendix, we derive components of the linearized Einstein tensor. Although similar formulae are derived in Appendix C in the Paper I [14] in the gauge-invariant form. However, in this paper, we have to derive the components of the Einstein tensor with the spherically background spacetime without any gauge fixing. In this case, the formulation of the “gauge-ready formulation” proposed in Ref. [58] in the context of cosmological perturbation theories is an appropriate formulation. Therefore, in this Appendix, we derive the components of the linear-order Einstein tensor without any gauge fixing following the philosophy of the “gauge-ready formulation” ’in Ref. [58]. The derived formulae in the philosophy of “gauge ready formulation” is useful in the ingredient of this manuscript.

Here, we consider the metric perturbation as

\begin{matrix} {}_{X} {\bar{g}}_{a b} = g_{a b} + ϵ {}_{X} h_{a b} + O (ϵ^{2}) . \end{matrix}

(A1)

The connection

C_{a b}^{c}

between the covariant derivative

{\bar{\nabla}}_{a}

associated with the metric

{\bar{g}}_{a b}

and the covariant derivative

\nabla_{a}

associated with the metric

g_{a b}

is given by

\begin{matrix} C_{a b}^{c} = \frac{1}{2} {\bar{g}}^{c d} (\nabla_{a} {\bar{g}}_{d b} + \nabla_{b} {\bar{g}}_{d a} - \nabla_{d} {\bar{g}}_{a b}), \end{matrix}

(A2)

where

{\bar{g}}^{a b}

is the inverse of

{\bar{g}}_{a b}

. Here, we expand the connection

C_{a b}^{c}

with respect to

ϵ

\begin{matrix} C_{a b}^{c} = ϵ {}^{(1)} C_{a b}^{c} + O (ϵ^{2}) . \end{matrix}

(A3)

Then, we have

\begin{matrix} {}^{(1)} C_{a b}^{c} = \frac{1}{2} g^{c d} (\nabla_{a} h_{d b} + \nabla_{b} h_{d a} - \nabla_{d} h_{a b}) . \end{matrix}

(A4)

The relation between the Riemann curvature

{\bar{R}}_{a b c}^{d}

associated with the metric

{\bar{g}}_{a b}

and the curvature

R_{a b c}^{d}

associated with the background metric

g_{a b}

is given by

\begin{matrix} {\bar{R}}_{a b c}^{d} = R_{a b c}^{d} - 2 \nabla_{[a} C_{b] c}^{d} + 2 C_{c [a}^{e} C_{b] e}^{d}, \end{matrix}

(A5)

Then, we have

\begin{matrix} {\bar{R}}_{a b c}^{d} = R_{a b c}^{d} - 2 ϵ \nabla_{[a} {}^{(1)} C_{b] c}^{d} + O (ϵ^{2}) . \end{matrix}

(A6)

The perturbative expansion of the Ricci tensor

{\bar{R}}_{a c}

is given by

\begin{matrix} {\bar{R}}_{a c} = R_{a c} - 2 ϵ \nabla_{[a} {}^{(1)} C_{b] c}^{b} + O (ϵ^{2}) . \end{matrix}

(A7)

The perturbative expansion of the curvature

{\bar{R}}_{a}^{c}

is given by

\begin{matrix} {\bar{R}}_{a}^{d} & = & {\bar{g}}^{c d} {\bar{R}}_{a c} \\ = & {\bar{g}}^{c d} {\bar{R}}_{a c} + ϵ (- 2 g^{c d} \nabla_{[a} {}^{(1)} C_{b] c}^{b} - h^{c d} R_{a c}) + O (ϵ^{2}) . \end{matrix}

(A8)

The perturbation of the scalar curvature is given by

\begin{matrix} \bar{R} & = & {\bar{g}}^{a c} {\bar{R}}_{a c} \\ = & R + ϵ (- h^{a c} R_{a c} - 2 g^{a c} \nabla_{[a} {}^{(1)} C_{b] c}^{b}) + O (ϵ^{2}) . \end{matrix}

(A9)

Then, the perturbative expansion of the Einstein tensor

{\bar{G}}_{a}^{d}

is given by

\begin{matrix} {\bar{G}}_{a}^{d} & = & {\bar{R}}_{a}^{d} - \frac{1}{2} δ_{a}^{d} \bar{R} \\ = & G_{a}^{d} + ϵ (- 2 g^{c d} \nabla_{[a} {}^{(1)} C_{b] c}^{b} + δ_{a}^{d} g^{e c} \nabla_{[e} {}^{(1)} C_{b] c}^{b} - h^{c d} R_{a c} + \frac{1}{2} δ_{a}^{d} h^{e c} R_{e c}) + O (ϵ^{2}) \\ = : & G_{a}^{d} + ϵ {}^{(1)} G_{a}^{d} + O (ϵ^{2}) . \end{matrix}

(A10)

Namely, the 1st-order perturbation of the Einstein tensor is given by

\begin{matrix} {}^{(1)} G_{a}^{d} & = & - 2 g^{c d} \nabla_{[a} {}^{(1)} C_{b] c}^{b} + δ_{a}^{d} g^{e c} \nabla_{[e} {}^{(1)} C_{b] c}^{b} - h^{c d} R_{a c} + \frac{1}{2} δ_{a}^{d} h^{e c} R_{e c} . \end{matrix}

(A11)

Substituting Equation (A4) into Equation (A11), we obtain

\begin{matrix} {}^{(1)} G_{a}^{d} & = & - \frac{1}{2} \nabla_{b} \nabla^{b} h_{a}^{d} + R_{a b c}^{d} h^{b c} \\ + \frac{1}{2} (g_{a c} \nabla^{d} - 2 δ_{[a}^{d} \nabla_{c]}) \nabla_{b} h^{c b} - \frac{1}{2} (\nabla_{a} \nabla^{d} - δ_{a}^{d} \nabla_{c} \nabla^{c}) h_{b}^{b} \\ - \frac{1}{2} R_{a c} h^{d c} + \frac{1}{2} R^{d f} h_{a f} + \frac{1}{2} δ_{a}^{d} h^{e c} R_{e c} . \end{matrix}

(A12)

Since we consider the vacuum background spacetime

R_{a b} = 0

, we obtain

\begin{matrix} {}^{(1)} G_{a}^{d} & = & - \frac{1}{2} \nabla_{b} \nabla^{b} h_{a}^{d} + R_{a b c}^{d} h^{b c} \\ + \frac{1}{2} (g_{a c} \nabla^{d} - 2 δ_{[a}^{d} \nabla_{c]}) \nabla_{b} h^{c b} - \frac{1}{2} (\nabla_{a} \nabla^{d} - δ_{a}^{d} \nabla_{c} \nabla^{c}) h_{b}^{b} . \end{matrix}

(A13)

To derive the component of

{}^{(1)} G_{a}^{d}

, we denote the components of the metric perturbation and the derivative operator as

\begin{matrix} {\bar{h}}_{A B} : = h_{A B}, {\bar{h}}_{A}^{D} : = y^{D E} h_{A E}, {\bar{h}}^{p D} : = γ^{p q} y^{D E} h_{q E}, \\ {\bar{h}}_{p}^{q} : = γ^{q r} h_{p r}, {\bar{h}}^{p q} : = γ^{p r} γ^{q s} h_{r s}, \end{matrix}

(A14)

and

\begin{matrix} {\bar{D}}^{C} = y^{C E} {\bar{D}}_{E}, {\hat{D}}^{p} = γ^{p q} {\hat{D}}_{q} . \end{matrix}

(A15)

Now, the components of

{}^{(1)} G_{a}^{d}

in terms of the variable defined by Equation (A14) as follows:

\begin{matrix} {}^{(1)} G_{A}^{B} & = & - \frac{1}{2} {\bar{D}}_{C} {\bar{D}}^{C} {\bar{h}}_{A}^{B} - \frac{1}{2 r^{2}} {\hat{D}}_{p} {\hat{D}}^{p} {\bar{h}}_{A}^{B} - \frac{2}{r^{2}} ({\bar{D}}^{C} r) ({\bar{D}}_{C} r) {\bar{h}}_{A}^{B} + \frac{2}{r^{2}} {\bar{h}}_{A}^{B} \\ + \frac{1}{2} {\bar{D}}^{B} {\bar{D}}^{C} {\bar{h}}_{A C} + \frac{1}{2} {\bar{D}}_{A} {\bar{D}}_{C} {\bar{h}}^{B C} - \frac{1}{r} ({\bar{D}}^{C} r) {\bar{D}}_{C} {\bar{h}}_{A}^{B} - \frac{1}{2} {\bar{D}}_{A} {\bar{D}}^{B} {\bar{h}}_{C}^{C} \\ + \frac{1}{r} ({\bar{D}}^{C} r) {\bar{D}}^{B} {\bar{h}}_{A C} + \frac{1}{r} ({\bar{D}}_{C} r) {\bar{D}}_{A} {\bar{h}}^{B C} \\ + \frac{1}{2 r^{2}} {\bar{D}}^{B} {\hat{D}}^{p} {\bar{h}}_{A p} + \frac{1}{2 r^{2}} {\bar{D}}_{A} {\hat{D}}_{p} {\bar{h}}^{B p} \\ - \frac{1}{2 r^{2}} {\bar{D}}_{A} {\bar{D}}^{B} {\bar{h}}_{r}^{r} + \frac{1}{2 r^{3}} ({\bar{D}}_{A} r) {\bar{D}}^{B} {\bar{h}}_{r}^{r} + \frac{1}{2 r^{3}} ({\bar{D}}^{B} r) {\bar{D}}_{A} {\bar{h}}_{r}^{r} - \frac{1}{r^{4}} ({\bar{D}}_{A} r) ({\bar{D}}^{B} r) {\bar{h}}_{r}^{r} \\ + y_{A}^{B} (- \frac{1}{2} {\bar{D}}_{C} {\bar{D}}_{D} {\bar{h}}^{C D} + \frac{1}{2} {\bar{D}}_{C} {\bar{D}}^{C} {\bar{h}}_{D}^{D} + \frac{1}{2 r^{2}} {\hat{D}}_{p} {\hat{D}}^{p} {\bar{h}}_{C}^{C} - \frac{2}{r} ({\bar{D}}_{D} r) {\bar{D}}_{C} {\bar{h}}^{C D} \\ + \frac{1}{r} ({\bar{D}}^{C} r) {\bar{D}}_{C} {\bar{h}}_{D}^{D} - \frac{1}{r^{2}} ({\bar{D}}_{C} r) ({\bar{D}}_{D} r) {\bar{h}}^{C D} + \frac{3}{2 r^{2}} ({\bar{D}}^{D} r) ({\bar{D}}_{D} r) {\bar{h}}_{C}^{C} \\ - \frac{1}{r^{2}} {\bar{D}}_{C} {\hat{D}}_{p} {\bar{h}}^{p C} - \frac{1}{r^{3}} ({\bar{D}}_{C} r) {\hat{D}}_{p} {\bar{h}}^{C p} \\ + \frac{1}{2 r^{2}} {\bar{D}}_{C} {\bar{D}}^{C} {\bar{h}}_{r}^{r} + \frac{1}{2 r^{4}} {\hat{D}}_{p} {\hat{D}}^{p} {\bar{h}}_{r}^{r} - \frac{1}{2 r^{3}} ({\bar{D}}^{C} r) {\bar{D}}_{C} {\bar{h}}_{r}^{r} - \frac{1}{2 r^{4}} {\hat{D}}_{p} {\hat{D}}_{s} {\bar{h}}^{p s} \\ + \frac{1}{2 r^{4}} ({\bar{D}}_{C} r) ({\bar{D}}^{C} r) {\bar{h}}_{r}^{r} - \frac{3}{2 r^{2}} {\bar{h}}_{C}^{C}) . \end{matrix}

(A16)

\begin{matrix} {}^{(1)} G_{A}^{q} & = & \frac{1}{2 r^{2}} {\hat{D}}^{q} {\bar{D}}^{C} {\bar{h}}_{A C} - \frac{1}{2 r^{2}} {\bar{D}}_{A} {\hat{D}}^{q} {\bar{h}}_{C}^{C} + \frac{1}{2 r^{3}} ({\bar{D}}_{A} r) {\hat{D}}^{q} {\bar{h}}_{C}^{C} \\ - \frac{1}{2 r^{2}} {\bar{D}}_{C} {\bar{D}}^{C} {\bar{h}}_{A}^{q} - \frac{1}{2 r^{4}} {\hat{D}}_{r} {\hat{D}}^{r} {\bar{h}}_{A}^{q} + \frac{1}{2 r^{4}} {\bar{h}}_{A}^{q} + \frac{1}{2 r^{4}} {\hat{D}}^{q} {\hat{D}}^{p} {\bar{h}}_{A p} \\ + \frac{1}{2 r^{2}} {\bar{D}}_{A} {\bar{D}}_{D} {\bar{h}}^{q D} - \frac{1}{r^{3}} ({\bar{D}}_{A} r) {\bar{D}}_{D} {\bar{h}}^{q D} - \frac{1}{r^{4}} ({\bar{D}}_{A} r) ({\bar{D}}_{D} r) {\bar{h}}^{q D} + \frac{1}{r^{3}} ({\bar{D}}_{D} r) {\bar{D}}_{A} {\bar{h}}^{q D} \\ + \frac{1}{2 r^{4}} {\bar{D}}_{A} {\hat{D}}_{s} {\bar{h}}^{q s} - \frac{1}{r^{5}} ({\bar{D}}_{A} r) {\hat{D}}_{s} {\bar{h}}^{q s} - \frac{1}{2 r^{4}} {\bar{D}}_{A} {\hat{D}}^{q} {\bar{h}}_{r}^{r} + \frac{1}{r^{5}} ({\bar{D}}_{A} r) {\hat{D}}^{q} {\bar{h}}_{r}^{r}, \end{matrix}

(A17)

\begin{matrix} {}^{(1)} G_{p}^{q} & = & - \frac{1}{2 r^{2}} {\bar{D}}_{C} {\bar{D}}^{C} {\bar{h}}_{p}^{q} - \frac{1}{2 r^{4}} {\hat{D}}_{s} {\hat{D}}^{s} {\bar{h}}_{p}^{q} + \frac{1}{r^{3}} ({\bar{D}}_{C} r) {\bar{D}}^{C} {\bar{h}}_{p}^{q} - \frac{2}{r^{4}} ({\bar{D}}_{C} r) ({\bar{D}}^{C} r) {\bar{h}}_{p}^{q} + \frac{2}{r^{4}} {\bar{h}}_{p}^{q} \\ - \frac{1}{2 r^{2}} {\hat{D}}_{p} {\hat{D}}^{q} {\bar{h}}_{C}^{C} + \frac{1}{2 r^{2}} {\hat{D}}_{p} {\bar{D}}_{C} {\bar{h}}^{q C} + \frac{1}{2 r^{2}} {\hat{D}}^{q} {\bar{D}}^{C} {\bar{h}}_{p C} \\ + \frac{1}{2 r^{4}} {\hat{D}}_{p} {\hat{D}}_{r} {\bar{h}}^{q r} + \frac{1}{2 r^{4}} {\hat{D}}^{q} {\hat{D}}^{r} {\bar{h}}_{p r} - \frac{1}{2 r^{4}} {\hat{D}}_{p} {\hat{D}}^{q} {\bar{h}}_{r}^{r} \\ + γ_{p}^{q} (- \frac{1}{2} {\bar{D}}_{C} {\bar{D}}_{D} {\bar{h}}^{C D} - \frac{1}{r} ({\bar{D}}_{C} r) {\bar{D}}_{D} {\bar{h}}^{C D} + \frac{1}{2} {\bar{D}}_{C} {\bar{D}}^{C} {\bar{h}}_{D}^{D} + \frac{1}{2 r} ({\bar{D}}^{C} r) {\bar{D}}_{C} {\bar{h}}_{D}^{D} \\ + \frac{1}{2 r^{2}} {\hat{D}}_{s} {\hat{D}}^{s} {\bar{h}}_{C}^{C} - \frac{1}{r^{2}} {\bar{D}}_{C} {\hat{D}}_{r} {\bar{h}}^{C r} \\ - \frac{1}{2 r^{4}} {\hat{D}}_{r} {\hat{D}}_{s} {\bar{h}}^{s r} - \frac{3}{2 r^{4}} {\bar{h}}_{r}^{r} + \frac{1}{2 r^{2}} {\bar{D}}_{C} {\bar{D}}^{C} {\bar{h}}_{r}^{r} - \frac{1}{r^{3}} ({\bar{D}}^{C} r) {\bar{D}}_{C} {\bar{h}}_{r}^{r} \\ + \frac{2}{r^{4}} ({\bar{D}}_{C} r) ({\bar{D}}^{C} r) {\bar{h}}_{r}^{r} + \frac{1}{2 r^{4}} {\hat{D}}_{s} {\hat{D}}^{s} {\bar{h}}_{r}^{r}) . \end{matrix}

(A18)

References

LIGO Scientific Collaboration 2024 home page: https://www.ligo.org/.
Virgo 2024 home page : https://www.virgo-gw.eu/.
KAGRA 2024 home page: https://gwcenter.icrr.u-tokyo.ac.jp/en/.
LIGO INDIA 2024 home page : https://www.ligo-india.in/.
Einstein Telescope 2024 home page : https://www.et-gw.eu/.
Cosmic Explorer 2024 home page : https://cosmicexplorer.org/.
LISA 2024 home page : https://lisa.nasa.gov/.
Kawamura, et al., Theor. Exp. Phys. 2021, 2021, 05A105.
J. Mei, et al. Theor. Exp. Phys. 2020, 2020, 05A107.
Z. Luo, et al., Theor. Exp. Phys. 2020, 2020, 05A108.
L. Barack and A. Pound. Rep. Prog. Phys. 2019; 82, 016904.
K. Nakamura, “Proposal of a gauge-invariant treatment of l=0,1-mode perturbations on Schwarzschild background spacetime”, Class. Quantum Grav. 2021, 38, 145010. [CrossRef]
K. Nakamura, “Formal Solutions of Any-Order Mass, Angular-Momentum, anda Dipole Perturbations on the Schwarzschild Background Spacetime”, Letters in High Energy Physics 2021 (2021), 215.
K. Nakamura, “Gauge-invariant perturbation theory on the Schwarzschild background spacetime Part I: — Formulation and odd-mode perturbations —”. arXiv:2110.13408v8 [gr-qc].
K. Nakamura, “Gauge-invariant perturbation theory on the Schwarzschild background spacetime Part II: — Even-mode perturbations —”. arXiv:2110.13512v5 [gr-qc].
K. Nakamura, “Gauge-invariant perturbation theory on the Schwarzschild background spacetime Part III: — Realization of exact solutions —”. arXiv:2110.13519v5 [gr-qc].
T. Regge and J. A. Wheeler, Phys. Rev. 108 (1957), 1063.
F. Zerilli, Phys. Rev. Lett. 24 (1970), 737.
F. Zerilli, Phys. Rev. D 2 (1970), 2141.
H. Nakano, Private note on “Regge-Wheeler-Zerilli formalism” (2019).
V. Moncrief, Ann. Phys. (N.Y.) 88 (1974), 323.
V. Moncrief, Ann. Phys. (N.Y.) 88 (1974), 343.
C. T. Cunningham, R. H. Price, and V. Moncrief, Astrophys. J. 224 (1978), 643.
S. Chandrasekhar, The mathematical theory of black holes (Oxford: Clarendon Press, 1983).
U.H. Gerlach and U.K. Sengupta, Phys. Rev. D 19 (1979), 2268.
U.H. Gerlach and U.K. Sengupta, Phys. Rev. D 20 (1979), 3009.
U.H. Gerlach and U.K. Sengupta, J. Math. Phys. 20 (1979), 2540.
U.H. Gerlach and U.K. Sengupta, Phys. Rev. D 22 (1980), 1300.
T. Nakamura, K. Oohara, Y. Kojima, Prog. Theor. Phys. Suppl. No. 90 (1987), 1.
C. Gundlach and J.M. Martín-García, Phys. Rev. D61 (2000), 084024.
J.M. Martín-García and C. Gundlach, Phys. Rev. D64 (2001), 024012.
A. Nagar and L. Rezzolla, Class. Quantum Grav. 22 (2005), R167; Erratum ibid. 23 (2006), 4297.
K. Martel and E. Poisson, Phys. Rev. D 71 (2005), 104003.
K. Nakamura, Prog. Theor. Phys. 110, (2003), 723.
K. Nakamura, Prog. Theor. Phys. 113 (2005), 481.
K. Nakamura, Class. Quantum Grav. 28 (2011), 122001.
K. Nakamura, Int. J. Mod. Phys. D 21 (2012), 124004.
K. Nakamura, Prog. Theor. Exp. Phys. 2013 (2013), 043E02.
K. Nakamura, Class. Quantum Grav. 31 (2014), 135013.
K. Nakamura, Advances in Astronomy, 2010 (2010), 576273.
K. Nakamura, “Second-order Gauge-invariant Cosmological Perturbation Theory: Current Status Updated in 2019”, Chapter 1 in Theory and Applications of Physical Science, Vol.3 Ed. M. Rafatullah, (Book Publisher International, 2020), ISBN 978-93-89816-24-2 (Print); ISBN 978-93-89816-25-9 (eBook). arXiv:1912.12805 [gr-qc].
A. J. Christopherson, K. A. Malik, D. R. -Matravers, K. Nakamura, Class. Quantum Grav. 28 (2011), 225024.
K. Nakamura, Phys. Rev. D 74 (2006), 101301(R).
K. Nakamura, Prog. Theor. Phys. 117 (2007), 17.
K. Nakamura, ““Gauge” in General Relativity: – Second-order general relativistic gauge-invariant perturbation theory –”, in Lie Theory and its Applications in Physics VII ed. V. K. Dobrev et al, (Heron Press, Sofia, 2008).
K. Nakamura, Phys. Rev. D 80 (2009), 124021.
K. Nakamura, Prog. Theor. Phys. 121 (2009), 1321.
L. Landau and E. Lifshitz, The Classical Theory of Fields (Addison-Wesley, Reading, Mass., 1962).
W. Kinnersley and M. Walker, Phys. Rev. D 2 (1970), 1359.
J. B. Griffiths, P. Krtous, and J. Podolsky, Class. and Quantum Grav. 23 (2006), 6745.
R. K. Sachs, “Gravitational Radiation”, in Relativity, Groups and Topology ed. C. DeWitt and B. DeWitt, (New York: Gordon and Breach, 1964).
J. M. Stewart and M. Walker, Proc. R. Soc. London A 341 (1974), 49.
J. M. Stewart, Class. Quantum Grav. 7 (1990), 1169.
J. M. Stewart, Advanced General Relativity (Cambridge University Press, Cambridge, 1991).
M. Bruni, S. M. Bruni, S. Matarrese, S. Mollerach and S. Sonego, Class. Quantum Grav. 14 (1997), 2585.
M. Bruni and S. Sonego, Class. Quantum Grav. 16 (1999), L29.
S. Sonego and M. Bruni, Commun. Math. Phys. 193 (1998), 209.
H. Noh and J. Hwang, Phys. Rev. D 69 (2004), 104011.

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Comparing a Gauge-Invariant Formulation and a “Conventional Complete Gauge-Fixing Approach” for l = 0, 1 Mode Perturbations on the Schwarzschild Background Spacetime

Abstract

1. Introduction

2. Brief Review of a Gauge-Invariant Treatment of l = 0 , 1 Modes

2.1. General Framework of Gauge-Invariant Perturbation Theory

2.2. Linear perturbations on spherically symmetric background spacetime

2.3. l = 1 Odd-Mode Linearized Einstein Equations and Solutions

2.4. l = 0 , 1 even-mode linearized Einstein equations and solutions

2.4.1. l = 1 Even-Mode Solution

2.4.2. l = 0 Even-Mode Solution

3. Rule of Comparison and Gauge-Transformation Rules in a Conventional Gauge-Fixing

3.1. Metric Perturbations

3.2. Conventional gauge-transformation rules for l = 0 , 1 metric perturbations

3.2.1. l ≥ 2 Perturbations

3.2.2. l = 1 Perturbations

3.2.3. l = 0 Perturbations

4. l=1 Odd-Mode Perturbation in the Conventional Approach

5. l=1 Even-Mode Perturbation in the Conventional Approach

6. l=0 Mode Perturbation in the Conventional Approach

6.1. Einstein Equations for l = 0 Mode Perturbations

6.2. Gauge-Fixing for l = 0 Mode Perturbations

6.3. Component Expression of the Linearized l = 0 Gauge-Fixed field equations

6.4. Comparing with Lemaître-Olman-Bondi Solution

6.4.1. Perturbative expression of the LTB solution on Schwarzschild background spacetime

6.4.2. Expression of the Perturbative LTB Solution in Static Chart

7. Summary and Discussions

Funding

Acknowledgments

Conflicts of Interest

Abbreviations

Appendix A. Linearized Einstein Tensor

References

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2. Brief Review of a Gauge-Invariant Treatment of $l = 0, 1$ Modes

2.3. $l = 1$ Odd-Mode Linearized Einstein Equations and Solutions

2.4. $l = 0, 1$ even-mode linearized Einstein equations and solutions

2.4.1. $l = 1$ Even-Mode Solution

2.4.2. $l = 0$ Even-Mode Solution

3.2. Conventional gauge-transformation rules for $l = 0, 1$ metric perturbations

3.2.1. $l \geq 2$ Perturbations

3.2.2. $l = 1$ Perturbations

3.2.3. $l = 0$ Perturbations

6.1. Einstein Equations for $l = 0$ Mode Perturbations

6.2. Gauge-Fixing for $l = 0$ Mode Perturbations

6.3. Component Expression of the Linearized $l = 0$ Gauge-Fixed field equations