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I found an article by E. J. Copeland, D. J. Mulryne, N. J. Nunes, M. Shaeri that explains this, it's called Super-inflation in Loop Quantum Cosmology. This is part of the answer I wrote most the equations come from this article unless I cite otherwise. According to Loop Quantum Cosmology, in super inflation a smaller number of e-folds are required. This is ...


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Here's the horizon problem: Look at the sky. Look at one side of the sky. Then look at the other side of the sky. The light from one side has just now reached you, as has the light from the other side. When we look back to the earliest observable moments of the universe, the Cosmic Microwave Background (CMB), we do the same thing. We look at light that was ...


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It means, that the cosmological perturbations satisfy Gaussian initial conditions. This means, that the probability of the perturbation amplitude has a Gaussian shape about the mean value. Considering linear perturbation theory, the initial Gaussian probability distribution will remain Gaussian for all times, e.g. today. It means, that there is e.g. no ...



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