Abstract
Minimal chaotic models of D-term inflation predicts too large primordial tensor perturbations. Although it can be made consistent with observations utilizing higher order terms in the K\"ahler potential, expansion is not controlled in the absence of symmetries. We comprehensively study the conditions of K\"ahler potential for D-term plateau-type potentials and discuss its symmetry. They include the alpha-attractor model with a massive vector supermultiplet and its generalization leading to pole inflation of arbitrary order. We extend the models so that it can describe Coulomb phase, gauge anomaly is cancelled, and fields other than inflaton are stabilized during inflation. We also point out a generic issue for large-field D-term inflation that the masses of the non-inflaton fields tend to exceed the Planck scale.
Highlights
We have shown that simple models of D-term chaotic inflation do not fit the current data
We have revisited the D-term inflationary attractor models in this paper. These attractor models can be realized in the context of pole inflation with a second order pole in the kinetic term
We have seen the limitation on the structure of Kahler potential for D-term inflationary attractor models
Summary
We briefly review large field D-term inflation models and their problems. The overall magnitude of the density perturbation is reproduced for g ∼ 10−6, this U(1) group cannot be identified with the subgroup of the standard model gauge group Another model is given in appendix B, in which Kahler potential is expanded in terms of logarithm of inflaton field rather than the inflaton field itself. To the above example, it is possible for its prediction to lie within the Planck contour by utilizing higher order terms in the Kahler potential. The Kahler potential is not controlled by any symmetry, there is no reason to expect that higher-order terms do not make comparable contributions to the results, which poses some doubts about the predictability of the model. This assumption is not always justified, as we will see below
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