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Volumn 24, Issue 5, 1982, Pages 1193-1198

Newtonian gravity on the null cone

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Indexed keywords

EID: 36749117424 PISSN: 00222488 EISSN: None Source Type: Journal
DOI: 10.1063/1.525796 Document Type: Article

Times cited : (55)

References (28)

1
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4
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- Trautman, A.¹

6
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- in, edited by B. Hoffman.(Indiana U.P., Bloomington)
- (1966) Perspectives in Geometry and Relativity
- Trautman, A.¹

10
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- in (BI Hochschultaschenbücher, Mannheim).(Festschrift for P. Mittelstaedt), edited by J. Nitsch et al.
- (1981) Grundlagen probleme der Physik
- Ehlers, J.¹

11
- 0000768999
- There are various hybrid, but physically appealing, treatments of post‐Newtonian effects which retain the Minkowski background metric but take slow motion limits in such a way that Newtonian gravity appears to leading order in the equations of motion; cf. the masterful work of. It seems that such treatments might be reformulated, as an expansion in a single parameter λ. with a strict Newtonian limit.
- (1965) Astrophs. J , vol.142 , pp. 1488
- Chandrasekhar, S.¹

14
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- (1962) Proc. R. Soc. London Ser. A , vol.270 , pp. 103
- Sachs, R.K.¹

15
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- (1966) Phys. Rev , vol.150 , pp. 1039
- Tamburino, L.¹ Winicour, J.²

16
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- .(Princeton U.P., Princeton, NJ)
- (1925) Riemannian Geometry
- Eisenhart, L.P.¹

17
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- (1966) J. Math. Phys , vol.7 , pp. 863
- Newman, E.¹ Penrose, R.²

19
- 0000956325
- It thus appears that odd powers of λ necessarily arise in order to distinguish between incoming and outgoing radiation. A similar feature involving even and odd powers of [formula omitted] occurs in other expansion formalisms; cf.
- (1970) Astrophys. J , vol.160 , pp. 153
- Chandrasekhar, S.¹ Esposito, P.²

20
- 84952295114
- These are the components of Einstein’s equation not involvinguderivatives.

21
- 84952295109
- This version of the characteristic initial value problem is identical to that of Ref. 15, where the inner world tube is now taken to be the vertex world‐line. Details for the axisymmetric case are given in Ref. 12.

22
- 84952295108
- It is not necessary, but convenient, to fix the zero of [formula omitted] at the origin. The spatial gradient of [formula omitted] must vanish because the origin is freely falling.

23
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- Here we assume ρ has compact support. A different asymptotic analysis is necessary for cosmological situations; cf.
- (1969) Astrophys. J , vol.155 , pp. 105
- Ehlers, J.¹ Rienstra, W.²

25
- 84952295111
- The distinction between Φ and [formula omitted] is irrelevant in determining the shear.

28
- 84952295116
- Some justification for this interpretation follows from considering the analogous Newtonian limit of the special relativistic wave equation.

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