By Antonio Alfonso-Faus
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Extra resources for Aspects of Today´s Cosmology
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In the specific case under consideration, however, the final symmetry reduces the free functions to only one and the reference line element is written: dσ 2 = b 2 ( τ ) dτ2 + dl 2 (19) The function b of the cosmic time has been called gauge function in (Radicella, 2011) but this denomination is not entirely correct, since b does not correspond to a real freedom: since we assume that the deformation process is a real one, the way the correspondence between the 2 Times are expressed as lengths. 38 Aspects of Today´s Cosmology unstrained and the strained manifold is established depends on the two Lamé coefficients of space-time, under the assumption of local isotropy.
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