Abstract
We calculate the spectral index and tensor-to-scalar ratio for patch inflation defined by and , using the slow-roll expansion. The patch cosmology arising from the Gauss–Bonnetbraneworld consists of Gauss–Bonnet (GB), Randall–Sundrum (RS), and 4D generalrelativistic (GR) cosmological models. In this work, we choose large-field potentials ofV = V0ϕp to compare with the observational data. Since second-order corrections are rather small inthe slow-roll limit, the leading-order calculation is sufficient to compare with the data.Finally, we show that it is easier to discriminate between a quadratic potential and quarticpotential in the GB cosmological model rather than the GR or RS cosmological models.
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