Abstract
In a previous paper the equations of small cosmological perturbations of a theory of gravitation in flat space-time are derived. They are applied to a homogeneous, isotropic, nonsingular cosmological model with radiation, matter and background field. At the beginning of the universe small spherically symmetric inhomogeneities on almost all scales can arise by instability. Later on the density contrast of dust grows exponentially during a short time epoch. The solution during this time period is given analytically.
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References
Bardeen, J.M.: 1980, Phys. Rev. D 22, 1882.
Bonnor, W.B.: 1967, in: J. Ehlers (ed.), Relativity Theory and Astrophysics, Providence: Am. Math. Soc., 263.
Israelit, M.; Rose, B.; Dehnen, H.: Astrophys. Space Sci. 220, 39.
Padmanabhan, T.: 1993, Structure Formation in the Universe, Cambridge University Press.
Petry, W.: 1994, Astrophys. Space Sci. 222, 127.
Petry, W.: 1995, Astrophys. Space Sci. 234, 177.
Petry, W.: 1996, Astrophys. Space Sci. 235, 41.
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Petry, W. Spherically symmetric cosmological perturbation in a universe with background field. Astrophysics and Space Science 250, 297–311 (1997). https://doi.org/10.1023/A:1000452205231
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DOI: https://doi.org/10.1023/A:1000452205231