Summary
The transformation of the Hamilton action integral of general relativity under infinitesimal co-ordinate transformations is used to derive a tensorial conservation theorem for the gravitational field. The total gravitational field is split into two parts: a «background» field (assumed to be given) and a perturbative part. The resulting conservation theorem is exact, covariant and of the Poynting type,i.e. only first derivatives of the perturbative field appear in it.
Riassunto
Si usa la trasformazione dell’integrale d’azione di Hamilton della relatività generale rispetto a trasformazioni infinitesime delle coordinate per dedurre un teorema tensoriale di conservazione per il campo gravitazionale. Si divide il campo gravitazionale totale in 2 parti: un campo «di fondo» (che si suppone dato) e una parte perturbativa. Se ne ottiene un teorema di conservazione esatto, covariante e del tipo di Pointing; cioè in esso appaiono solo le derivate prime del campo perturbativo.
Режюме
Преобразование интеграла действия общей теории относительности при бесконечно малых преобразованиях координат используется для вывода тензорной теоремы сохранения для гравитационного поля. Полное гравитациное поле расщепляется на две части: «фоновое» поле (предполагается заданным) и пертурбационная часть. Полученная теорема сохранения является точной, ковариантной и имеет форму теоремы Пойнтинга, т.е. в ней появляются только первые производные пертурбационного поля.
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References
SeeP. Bergmann:Introduction to the Theory of Relativity (Englewood Cliffs, N. J., 1942).
P. Bergmann:Phys. Rev.,112, 287 (1958).
J. Goldberg:Phys. Rev.,89, 263 (1953);P. von Freund:Am. Math.,40, 417 (1939).
P. Bergman:loc. cit. SeeP. Bergmann:Introduction to the Theory of Relativity (Englewood Cliffs, N. J., 1942).
We use German letters to denote tensor densities. Thusg μν=ωg μν, whereω=(−detg μν )1/2, andg μν has signatureRu-+ when reduced to diagonal form.
ThusΓ λ μν,σ =∂Γ λ μν /∂x σ . Similarly, we use the semi-colon to denote covariant differentiation,e.g. g μν;σ =Γ μν,σ −g μϱ Γ ϱ νσ −g νϱ Γ ϱ μσ .
For a general method for computing these co-ordinate-induced variations seeH. Weyl:Space-Time-Matter (New York, N. Y., 1950).
The subscript (0) placed after an index of covariant differentiation means that the background field affine connectiongG ϱ μν(0) is to be used in computing it. ThusA μ;ν(0) =A μ;ν =A σ Γ μ σν(0) , etc.
This statement is necessarily somewhat imprecise since, due to the nonlinearity of the field equations, no unique division of the total field exists which can be attributed to contributions from separate sources.
A conservation theorem of this type for the special case where the background field is flat seems to have been first derived byN. Rosen:Phys. Rev.,57, 147 (1940).
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Ging, J.L., Ferrell, T.L. A covariant conservation theorem in general relativity. Nuov Cim B 24, 189–196 (1974). https://doi.org/10.1007/BF02725956
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DOI: https://doi.org/10.1007/BF02725956