2018
DOI: 10.18063/eoaa.v2i1.384
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Is Spacetime Non-metric?

Abstract: If one assumes higher dimensions and that dimensional reduction from higher dimensions produces scalar-tensor theory and also that Palatini variation is the correct method of varying scalar-tensor theory then spacetime is nonmetric. Palatini variation of Jordan frame lagrangians gives an equation relating the dilaton to the object of non-metricity and hence the existence of the dilaton implies that the spacetime connection is more general than that given soley by the Christoffel symbol of general relativity. T… Show more

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Cited by 4 publications
(5 citation statements)
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“…From the optical study of the kinematics of stars in the solar neighborhood, Bertil Lindblad (1927) and Jan Oort (1927) deduced that the flattening of the galactic disk is due to rotation, and that this rotation occurred differentially, with the stars near the galactic center taking less time to go once around the center than the material farther out. It was natural to ask whether the same held true for external disk galaxies, and in the late 1950s to early 1970s, optical and radio astronomers discovered that, instead of being in a state of uniform rotation, ( ) = constant, the outer rotation curves of normal and barred spiral galaxies were roughly flat; that is, ( ) = constant, where is the radial distance from the rotation axis in the plane of the disk and ( ) is the angular speed of rotation (Van de Hulst et al 1957, Rubin et al 1964, H öglund & Roberts 1965, Rubin & Ford 1970, Roberts & Rots 1973.…”
Section: Introduction and Historical Contextmentioning
confidence: 99%
“…From the optical study of the kinematics of stars in the solar neighborhood, Bertil Lindblad (1927) and Jan Oort (1927) deduced that the flattening of the galactic disk is due to rotation, and that this rotation occurred differentially, with the stars near the galactic center taking less time to go once around the center than the material farther out. It was natural to ask whether the same held true for external disk galaxies, and in the late 1950s to early 1970s, optical and radio astronomers discovered that, instead of being in a state of uniform rotation, ( ) = constant, the outer rotation curves of normal and barred spiral galaxies were roughly flat; that is, ( ) = constant, where is the radial distance from the rotation axis in the plane of the disk and ( ) is the angular speed of rotation (Van de Hulst et al 1957, Rubin et al 1964, H öglund & Roberts 1965, Rubin & Ford 1970, Roberts & Rots 1973.…”
Section: Introduction and Historical Contextmentioning
confidence: 99%
“…It should be noted that axial symmetry is not impossible but implies additional restrictions on the mass distribution. Because of the importance of axial symmetry in our Universe, particularly for galaxies, we perform a more detailed investigation in the next section [26].…”
Section: Non-relativistic Limitmentioning
confidence: 99%
“…To preserve the consistency of the theory, we can add only point mass M b at r = 0 (dashed line in figure 1(c)). The experimental data were obtained from [26,27]. The dash-dotted lines correspond to the classical Newtonian potential.…”
Section: Axial Symmetrymentioning
confidence: 99%
“…P : because the scalar-tensor theory involves Palatini variations the underlying geometry is no longer Riemannian but rather Weyl with object of nonmetricity related to the primary dilation function A, see [4].…”
Section: Properties and Commentsmentioning
confidence: 99%
“…From a Newtonian perspective the gravitational modification which works is the replacement of the Newtonian reciprocal gravitational potential by a logarithmic potential; the spherically symmetric relativistic generalization of this [3] has one free function which in the present work is fixed by requiring that the Weyl tensor vanishes. This leaves the problem of finding which field equations the Einstein tensor obeys and both Palatini varied scalar-tensor theory [4] and the low energy limit of string theory with added potential are found to work. The usual method of approaching problems is by starting with a Lagrangian, then deriving field equations, finding solutions, and finally comparing with observations; here this is reversed: in the present case it is observation, then metric, then field equations, and finally Lagrangian.…”
Section: Introductionmentioning
confidence: 99%