- Source: Post-Newtonian expansion
In general relativity, post-Newtonian expansions (PN expansions) are used for finding an approximate solution of Einstein field equations for the metric tensor. The approximations are expanded in small parameters that express orders of deviations from Newton's law of universal gravitation. This allows approximations to Einstein's equations to be made in the case of weak fields. Higher-order terms can be added to increase accuracy, but for strong fields sometimes it is preferable to solve the complete equations numerically. This method is a common mark of effective field theories. In the limit, when the small parameters are equal to 0, the post-Newtonian expansion reduces to Newton's law of gravity.
Expansion in 1/c2
The post-Newtonian approximations are expansions in a small parameter, which is the ratio of the velocity of the matter that creates the gravitational field, to the speed of light, which in this case is more precisely called the speed of gravity. In the limit, when the fundamental speed of gravity becomes infinite, the post-Newtonian expansion reduces to Newton's law of gravity. A systematic study of post-Newtonian expansions within hydrodynamic approximations was developed by Subrahmanyan Chandrasekhar and his colleagues in the 1960s.
Expansion in h
Another approach is to expand the equations of general relativity in a power series in the deviation of the metric from its value in the absence of gravity.
h
α
β
=
g
α
β
−
η
α
β
.
{\displaystyle h_{\alpha \beta }=g_{\alpha \beta }-\eta _{\alpha \beta }\,.}
To this end, one must choose a coordinate system in which the eigenvalues of
h
α
β
η
β
γ
{\displaystyle h_{\alpha \beta }\eta ^{\beta \gamma }\,}
all have absolute values less than 1.
For example, if one goes one step beyond linearized gravity to get the expansion to the second order in h:
g
μ
ν
≈
η
μ
ν
−
η
μ
α
h
α
β
η
β
ν
+
η
μ
α
h
α
β
η
β
γ
h
γ
δ
η
δ
ν
.
{\displaystyle g^{\mu \nu }\approx \eta ^{\mu \nu }-\eta ^{\mu \alpha }h_{\alpha \beta }\eta ^{\beta \nu }+\eta ^{\mu \alpha }h_{\alpha \beta }\eta ^{\beta \gamma }h_{\gamma \delta }\eta ^{\delta \nu }\,.}
−
g
≈
1
+
1
2
h
α
β
η
β
α
+
1
8
h
α
β
η
β
α
h
γ
δ
η
δ
γ
−
1
4
h
α
β
η
β
γ
h
γ
δ
η
δ
α
.
{\displaystyle {\sqrt {-g}}\approx 1+{\tfrac {1}{2}}h_{\alpha \beta }\eta ^{\beta \alpha }+{\tfrac {1}{8}}h_{\alpha \beta }\eta ^{\beta \alpha }h_{\gamma \delta }\eta ^{\delta \gamma }-{\tfrac {1}{4}}h_{\alpha \beta }\eta ^{\beta \gamma }h_{\gamma \delta }\eta ^{\delta \alpha }\,.}
Expansions based only on the metric, independently from the speed, are called post-Minkowskian expansions (PM expansions).
Uses
The first use of a PN expansion (to first order) was made by Albert Einstein in calculating the perihelion precession of Mercury's orbit. Today, Einstein's calculation is recognized as a common example of applications of PN expansions, solving the general relativistic two-body problem, which includes the emission of gravitational waves.
Newtonian gauge
In general, the perturbed metric can be written as
d
s
2
=
a
2
(
τ
)
[
(
1
+
2
A
)
d
τ
2
−
2
B
i
d
x
i
d
τ
−
(
δ
i
j
+
h
i
j
)
d
x
i
d
x
j
]
{\displaystyle ds^{2}=a^{2}(\tau )\left[(1+2A)d\tau ^{2}-2B_{i}dx^{i}d\tau -\left(\delta _{ij}+h_{ij}\right)dx^{i}dx^{j}\right]}
where
A
{\displaystyle A}
,
B
i
{\displaystyle B_{i}}
and
h
i
j
{\displaystyle h_{ij}}
are functions of space and time.
h
i
j
{\displaystyle h_{ij}}
can be decomposed as
h
i
j
=
2
C
δ
i
j
+
∂
i
∂
j
E
−
1
3
δ
i
j
◻
2
E
+
∂
i
E
^
j
+
∂
j
E
^
i
+
2
E
~
i
j
{\displaystyle h_{ij}=2C\delta _{ij}+\partial _{i}\partial _{j}E-{\frac {1}{3}}\delta _{ij}\Box ^{2}E+\partial _{i}{\hat {E}}_{j}+\partial _{j}{\hat {E}}_{i}+2{\tilde {E}}_{ij}}
where
◻
{\displaystyle \Box }
is the d'Alembert operator,
E
{\displaystyle E}
is a scalar,
E
^
i
{\displaystyle {\hat {E}}_{i}}
is a vector and
E
~
i
j
{\displaystyle {\tilde {E}}_{ij}}
is a traceless tensor.
Then the Bardeen potentials are defined as
Ψ
≡
A
+
H
(
B
−
E
′
)
,
+
(
B
+
E
′
)
′
,
Φ
≡
−
C
−
H
(
B
−
E
′
)
+
1
3
◻
E
{\displaystyle \Psi \equiv A+H(B-E'),+(B+E')',\quad \Phi \equiv -C-H(B-E')+{\frac {1}{3}}\Box E}
where
H
{\displaystyle H}
is the Hubble constant and a prime represents differentiation with respect to conformal time
τ
{\displaystyle \tau \,}
.
Taking
B
=
E
=
0
{\displaystyle B=E=0}
(i.e. setting
Φ
≡
−
C
{\displaystyle \Phi \equiv -C}
and
Ψ
≡
A
{\displaystyle \Psi \equiv A}
), the Newtonian gauge is
d
s
2
=
a
2
(
τ
)
[
(
1
+
2
Ψ
)
d
τ
2
−
(
1
−
2
Φ
)
δ
i
j
d
x
i
d
x
j
]
{\displaystyle ds^{2}=a^{2}(\tau )\left[(1+2\Psi )d\tau ^{2}-(1-2\Phi )\delta _{ij}dx^{i}dx^{j}\right]\,}
.
Note that in the absence of anisotropic stress,
Φ
=
Ψ
{\displaystyle \Phi =\Psi }
.
A useful non-linear extension of this is provided by the non-relativistic gravitational fields.
See also
Coordinate conditions
Einstein–Infeld–Hoffmann equations
Linearized gravity
Parameterized post-Newtonian formalism
References
External links
"On the Motion of Particles in General Relativity Theory" by A.Einstein and L.Infeld Archived 2012-03-08 at the Wayback Machine
Blanchet, Luc (2014). "Gravitational Radiation from Post-Newtonian Sources and Inspiralling Compact Binaries". Living Reviews in Relativity. 17 (1): 2. arXiv:1310.1528. Bibcode:2014LRR....17....2B. doi:10.12942/lrr-2014-2. PMC 5256563. PMID 28179846.
Clifford, M. Will (2011). "On the unreasonable effectiveness of thepost-Newtonian approximation ingravitational physics". PNAS. 108 (15): 5938–5945. arXiv:1102.5192. doi:10.1073/pnas.1103127108. PMC 3076827. PMID 21447714.
Kata Kunci Pencarian:
- Post-Newtonian expansion
- Two-body problem in general relativity
- Parameterized post-Newtonian formalism
- Sergei Kopeikin
- Post-Minkowskian expansion
- PN
- General relativity
- Gravity
- Non-relativistic gravitational fields
- Reduced mass
