Abstract
In Chaps. 4 and 5 we have derived the evolution equations for small fluctuations about the homogeneous and isotropic FLRW background. These equations are differential and so, in order to have a well-posed Cauchy problem, we need to know which initial conditions to use. This is the topic of this chapter, where we shall be concerned with scalar perturbations only. Many papers in the literature are concerned about initial conditions in cosmology, but we shall mainly refer to (Ma, and Bertschinger. Astrophys. J., 455, 7–25 (1995), Bucher, Moodley and Turok. Phys. Rev. D, 62, 083508 (2000)) Ma and Bertschinger (1995), Bucher et al. (2000).
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Notes
- 1.
There must be a typo in Eq. 28 of Bucher et al. (2000), since the gravitational potentials appear to be equal but they cannot be because of the presence of neutrinos and the quadrupole moment of their distribution.
References
Ade, P.A.R., et al.: Planck 2015 results XIII. Cosmological parameters. Astron. Astrophys. 594, A13 (2016a)
Ade, P.A.R., et al.: Planck 2015 results XX. Constraints on inflation. Astron. Astrophys. 594, A20 (2016c)
Bucher, M., Moodley, K., Turok, N.: The general primordial cosmic perturbation. Phys. Rev. D 62, 083508 (2000)
Ma, C.-P., Bertschinger, E.: Cosmological perturbation theory in the synchronous and conformal Newtonian gauges. Astrophys. J. 455, 7–25 (1995)
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Piattella, O. (2018). Initial Conditions. In: Lecture Notes in Cosmology. UNITEXT for Physics. Springer, Cham. https://doi.org/10.1007/978-3-319-95570-4_6
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