Abstract
We go a step further in the search for a consistent and realistic supergravity model of large-field inflation by building a class of models with the following features: during slow-roll, all the scalar fields other than the inflaton are frozen by large inflatondependent masses or removed from the spectrum; at the end of inflation, supersymmetry is spontaneously broken with naturally vanishing classical vacuum energy. We achieve this by combining some geometrical properties of the Kähler potential with the consistent use of a single nilpotent chiral superfield, in one-to-one correspondence with the supersymmetrybreaking direction in field space at the vacuum.
Highlights
The spectrum by imposing a supersymmetric quadratic constraint
We go a step further in the search for a consistent and realistic supergravity model of large-field inflation by building a class of models with the following features: during slow-roll, all the scalar fields other than the inflaton are frozen by large inflatondependent masses or removed from the spectrum; at the end of inflation, supersymmetry is spontaneously broken with naturally vanishing classical vacuum energy
We build a class of models where: during slow-roll, all the scalar fields other than the inflaton are either frozen by large inflaton-dependent masses or removed from the spectrum; the nilpotency constraint can be solved consistently on the full field space; at the end of inflation, supersymmetry is spontaneously broken with naturally vanishing classical vacuum energy, and the supersymmetry-breaking direction in field space is exactly aligned with the nilpotent multiplet
Summary
The inflaton field φ is usually identified with one of the two real scalar degrees of freedom of a chiral multiplet Φ, the inflaton multiplet. A minimal requirement for model building is that the slow-roll conditions are satisfied in the inflaton direction. Neglecting for a moment all the other scalar fields, the slow-roll conditions read ǫ. An initial difficulty in building supergravity models for large-field inflation fulfilling the slow-roll conditions (1.8) was the fact that the potential (1.3) is proportional to eK, to eφ in models with canonical Kahler potential K = |Φ|2 for the inflaton multiplet, which makes η of order one. It is well known that the way out [3] is to impose a shift symmetry on the inflaton Kahler potential. That the inflaton φ is the imaginary part of the complex scalar φ in Φ and that the corresponding shift symmetry in the Kahler potential translates into K = K(Φ + Φ)
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