Bimetric theory

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Bimetric theory refers to a class of modified mathematical theories of gravity (or gravitation) in which two metric tensors are used instead of one. Often the second metric is introduced at high energies, with the implication that the speed of light may be energy-dependent. There are several different bimetric theories, such as those attributed to Nathan Rosen (1909–1995)[1][2] or Mordehai Milgrom with Modified Newtonian Dynamics (MOND).[3] Though none has been shown to account for physical observations more accurately or more consistently than the theory of general relativity, Rosen's theory has been shown to be inconsistent with observations of the "Hulse–Taylor binary pulsar".[1]


In general relativity (GR), it is assumed that the distance between two points in spacetime is given by the metric tensor. Einstein's field equation is then used to calculate the form of the metric based on the distribution of energy and momentum.

Rosen (1940) has proposed that at each point of space-time, there is a Euclidean metric tensor \gamma_{ij} in addition to the Riemannian metric tensor g_{ij} . Thus at each point of space-time there are two metrics:


2.~~~~d\sigma^{2}=\gamma_{ij} dx^{i} dx^{j}

The first metric tensor, g_{ij} , describes the geometry of space-time and thus the gravitational field. The second metric tensor, \gamma_{ij} , refers to the flat space-time and describes the inertial forces. The Christoffel symbols formed from g_{ij} and \gamma_{ij} are denoted by \{^{i}_{jk}\} and \Gamma^{i}_{jk} respectively. The quantities \Delta are defined such that


Two kinds of covariant differentiation then arise: g-differentiation based on g_{ij} (denoted by a semicolon), and 3-differentiation based on \gamma_{ij} (denoted by a slash). Ordinary partial derivatives are represented by a comma. Let R^{\lambda}_{ij \sigma} and P^{\lambda}_{ij \sigma} be the Riemann curvature tensors calculated from g_{ij} and \gamma_{ij}, respectively. In the above approach the curvature tensor P^{\lambda}_{ij \sigma} is zero, since \gamma_{ij} is the flat space-time metric.

From (1) one finds that though {:} and \Gamma are not tensors, but \Delta is a tensor having the same form as {:} except that the ordinary partial derivative is replaced by 3-covariant derivative. A straightforward calculation yields the Riemann curvature tensor


Each term on right hand side is a tensor. It is seen that from GR one can go to the new formulation just by replacing {:} by \Delta, ordinary differentiation by 3-covariant differentiation, \sqrt {-g} by \sqrt{\frac{g}{\gamma}}, integration measure d^{4}x by \sqrt {-\gamma}d^{4}x, where g = det(g_{ij}), 3 = det(\gamma_{ij}) and d^{4}x = dx^{1}dx^{2}dx^{3}dx^{4}. Having once introduced \gamma_{ij} into the theory, one has a great number of new tensors and scalars at one's disposal. One can set up other field equations other than Einstein's. It is possible that some of these will be more satisfactory for the description of nature.

The geodesic equation in bimetric relativity (BR) takes the form


It is seen from equations (1) and (2) that \Gamma can be regarded as describing the inertial field because it vanishes by a suitable coordinate transformation.

The quantity \Delta, being a tensor, is independent of any coordinate system and hence may be regarded as describing the permanent gravitational field.

Rosen (1973) has found BR satisfying the covariance and equivalence principle. In 1966, Rosen showed that the introduction of the space metric into the framework of general relativity not only enables one to get the energy momentum density tensor of the gravitational field, but also enables one to obtain this tensor from a variational principle. The field equations of BR derived from the variational principle are

K^{i}_{j}= N^{i}_{j}-\frac{1}{2}\delta^{i}_{j}N = -8 \pi \kappa T^{i}_{j}~~~~~~~~~~~~~~(3)


N^{i}_{j}=\frac{1}{2}\gamma^{\alpha \beta}(g^{hi} g_{hj /\alpha})_{/ \beta}


N^{i}_{j}=\frac{1}{2} \gamma^{\alpha \beta}\Big\{(g^{hi}g_{hj, \alpha})_{,\beta }
- (g^{hi}g_{mj}\Gamma^{m}_{h\alpha})_{,\beta} 
-\gamma^{\alpha \beta}(\Gamma^{i}_{j\alpha})_{,\beta}
 + \Gamma^{i}_{\lambda \beta}[g^{h\lambda}g_{hj,\alpha} - g^{h\lambda}g_{mj}\Gamma^{m}_{h\alpha}- \Gamma^{\lambda}_{j\alpha}]\\
\qquad -\Gamma^{\lambda}_{j\beta}[g^{hi}g_{h\lambda,\alpha} - g^{hi}g_{m\lambda}\Gamma^{m}_{h\alpha} -\Gamma^{i}_{\lambda\alpha}]
 + \Gamma^{\lambda}_{\alpha \beta}[g^{hi}g_{hj,\lambda} - g^{hi}g_{mj}\Gamma^{m}_{h\lambda} -\Gamma^{i}_{j\lambda}]\Big\}

N= g^{ij}N_{ij}, \qquad \kappa=\sqrt{\frac{g}{\gamma}},

and T^{i}_{j} is the energy-momentum tensor.

The variational principle also leads to the relation


Hence from (3)


which implies that in a BR, a test particle in a gravitational field moves on a geodesic with respect to g_{ij}.

It is found that the BR and GR theories differ in the following cases:

  • propagation of electromagnetic waves
  • the external field of a high density star
  • the behaviour of intense gravitational waves propagating through a strong static gravitational field.

The predictions of gravitational radiation in Rosen's theory have been shown to be in conflict with observations of the "Hulse–Taylor binary pulsar".[1] Note that other bimetric gravitational theories exist.


  1. ^ a b c The New Physics, Paul Davies, 1992, 526 pages, web: Books-Google-ak.
  2. ^ "Nathan Rosen — The Man and His Life-Work",, 2011, web: Technion-rosen.
  3. ^ Reinventing gravity: a physicist goes beyond Einstein, John W. Moffat, 2008, 272 pages, p.103, webpage: BG-6K.

External links[edit]

Bimetric Theory of Gravitational-Inertial Field in Riemannian and in Finsler-Lagrange Approximation Authors: J.Foukzon, S.A.Podosenov, A.A.Potapov, E.Menkova