1. Cosimo Stornaiolo INFN-Sezione di Napoli MG 12 Paris 12-18 July 2009

2. D. Pugliese, Deformazioni di metriche spazio-temporali, tesi di laurea quadriennale, relatori S. Capozziello e C. Stornaiolo S. Capozziello e C. Stornaiolo, Space-Time deformations as extended conformal transformations International Journal of Geometric Methods in Modern Physics 5, 185-196 (2008)

3. In General Relativity, we usually deal with Exact solutions to describe cosmology, black holes, motions in the solar system, astrophysical objects Approximate solutions to deal with gravitational waves, gravitomagnetic effects, cosmological perturbations, post-newtonian parametrization Numerical simulations In General Relativity, we usually deal with Exact solutions to describe cosmology, black holes, motions in the solar system, astrophysical objects Approximate solutions to deal with gravitational waves, gravitomagnetic effects, cosmological perturbations, post-newtonian parametrization Numerical simulations

4. Nature of dark matter and of dark energy Unknown distribution of (dark) matter and (dark) energy Pioneer anomaly Relation of the geometries between the different scales Which theory describes best gravitation at different scales Alternative theories Approximate symmetries or complete lack of symmetry Spacetime inhomogeneities Boundary conditions Initial conditions Nature of dark matter and of dark energy Unknown distribution of (dark) matter and (dark) energy Pioneer anomaly Relation of the geometries between the different scales Which theory describes best gravitation at different scales Alternative theories Approximate symmetries or complete lack of symmetry Spacetime inhomogeneities Boundary conditions Initial conditions

5. Let us try to define a general covariant way to deal with the previous list of problems. In an arbitrary space time, an exact solution of Einstein equations, can only describe in an approximative way the real structure of the spacetime geometry. Our purpose is to encode our ignorance of the correct spacetime geometry by deforming the exact solution with scalar fields. Let us see how……… Let us try to define a general covariant way to deal with the previous list of problems. In an arbitrary space time, an exact solution of Einstein equations, can only describe in an approximative way the real structure of the spacetime geometry. Our purpose is to encode our ignorance of the correct spacetime geometry by deforming the exact solution with scalar fields. Let us see how………

6. Let us consider the surface of the earth, we can consider it as a (rotating) sphere But this is an approximation Let us consider the surface of the earth, we can consider it as a (rotating) sphere But this is an approximation

7. Measurments indicate that the earth surface is better described by an oblate ellipsoid Mean radius 6,371.0 km Equatorial radius 6,378.1 kmEquatorial Polar radius 6,356.8 kmPolar Flattening 0.0033528Flattening But this is still an approximation Measurments indicate that the earth surface is better described by an oblate ellipsoid Mean radius 6,371.0 km Equatorial radius 6,378.1 kmEquatorial Polar radius 6,356.8 kmPolar Flattening 0.0033528Flattening But this is still an approximation

8. We can improve our measurements an find out that the shape of the earth is not exactly described by any regular solid. We call the geometrical solid representing the Earth a geoid 1. Ocean 2. Ellipsoid 3. Local plumb 4. Continent 5. Geoid

11. It is well known that all the two dimensional metrics are related by conformal transformations, and are all locally conform to the flat metric

12. The question is if there exists an intrinsic and covariant way to relate similarly metrics in dimensions

13. In an n-dimensional manifold with metric the metric has degrees of freedom In an n-dimensional manifold with metric the metric has degrees of freedom

14. In 2002 Coll, Llosa and Soler (General Relativity and Gravitation, Vol. 34, 269, 2002) showed that any metric in a 3D space(time) is related to a constant curvature metric by the following relation

15. Question: How can we generalize the conformal transformations in 2 dimensions an Coll and coworkers deformation in 3 dimensions to more than 3 dimension spacetimes ?

16. Let us see if we can generalize the preceding result possibly expressing the deformations in terms of scalar fields as for conformal transformations. What do we mean by metric deformation? Let us first consider the decomposition of a metric in tetrad vectors

19. The deformation matrices are the corrections of exact solutions to consider a realistic spacetime They are the unknown of our problem  They can be obtained by phenomenolgical observations  Or even as solutions of a set of differential equations The deformation matrices are the corrections of exact solutions to consider a realistic spacetime They are the unknown of our problem  They can be obtained by phenomenolgical observations  Or even as solutions of a set of differential equations

20. are matrices of scalar fields in spacetime, Deforming matrices are scalars with respect to coordinate transformations. are matrices of scalar fields in spacetime, Deforming matrices are scalars with respect to coordinate transformations.

21. A particular class of deformations is given by which represent the conformal transformations This is one of the first examples of deformations known from literature. For this reason we can consider deformations as an extension of conformal transformations. A particular class of deformations is given by which represent the conformal transformations This is one of the first examples of deformations known from literature. For this reason we can consider deformations as an extension of conformal transformations.

22.  Conformal transformations given by a change of coordinates flat (and open) Friedmann metrics and Einsteiin (static) universe  Conformal transformation that cannot be obtained by a change of coordinates closed Friedmann metric

23. If the metric tensors of two spaces and are related by the relation we say that is the deformation of (cfr. L.P. Eisenhart, Riemannian Geometry, pag. 89) If the metric tensors of two spaces and are related by the relation we say that is the deformation of (cfr. L.P. Eisenhart, Riemannian Geometry, pag. 89)

24. They are not necessarily real They are not necessarily continuos (so that we may associate spacetimes with different topologies) They are not coordinate transformations (one should transform correspondingly all the covariant and contravariant tensors), i.e. they are not diffeomorphisms of a spacetime M to itself They can be composed to give successive deformations They may be singular in some point, if we expect to construct a solution of the Einstein equations from a Minkowski spacetime They are not necessarily real They are not necessarily continuos (so that we may associate spacetimes with different topologies) They are not coordinate transformations (one should transform correspondingly all the covariant and contravariant tensors), i.e. they are not diffeomorphisms of a spacetime M to itself They can be composed to give successive deformations They may be singular in some point, if we expect to construct a solution of the Einstein equations from a Minkowski spacetime

26. By lowering its index with a Minkowski matrix we can decompose the first deforming matrix

27. Substituting in the expression for deformation the second deforming matrix takes the form Inserting the tetrad vectors to obtain the metric it follows that (next slide) Substituting in the expression for deformation the second deforming matrix takes the form Inserting the tetrad vectors to obtain the metric it follows that (next slide)

28. Reconstructing a deformed metric leads to This is the most general relation between two metrics. This is the third way to define a deformation

29. To complete the definition of a deformation we need to define the deformation of the corresponding contravariant tensor

30. We are now able to define the connections where and is a tensor We are now able to define the connections where and is a tensor

31. Finally we can define how the curvature tensors are deformed

32. The equations in the vacuum take the form

33. In presence of matter sources the equations for the deformed metric are of the form

34.  Conformal transformations  Kerr-Schild metrics  Metric perturbations: cosmological perturbations and gravitational waves

35. In our approach the approximation is given by the conditions This conditions are covariant for three reasons: 1) we are using scalar fields; 2) this objects are adimensional; 3) they are subject only to Lorentz transformations; In our approach the approximation is given by the conditions This conditions are covariant for three reasons: 1) we are using scalar fields; 2) this objects are adimensional; 3) they are subject only to Lorentz transformations;

38. The gauge conditions are no more coordinate conditions. instead they are restrictions in the choice of the perturbing scalars.

39. We have presented the deformation of spacetime metrics as the corrections one has to introduce in the metric in order to deal with our ignorance of the fine spacetime structure. The use of scalars to define deformation can simplify many conceptual issues As a result we showed that we can consider a theory of no more than six scalar potentials given in a background geometry We showed that this scalar field are suitable for a covariant definition for the cosmological perturbations and also for gravitational waves Using deformations we can study covariantly the Inhomogeneity and backreaction problems Cosmological perturbations but also Gravitational waves in arbitrary spacetimes Symmetry and approximate symmetric properties of spacetime The boundary and initial conditions The relation between GR and alternative gravitational theories