We consider a power law 1 M 2 R β correction to Einstein gravity as a model for inflation. The interesting feature of this form of generalization is that small deviations from the Starobinsky limit β = 2 can change the value of tensor-to-scalar ratio from r ～ O ( 10 ? 3 ) to r ～ O ( 0.1 ) . We find that in order to get large tensor perturbation r ≈ 0.1 as indicated by BKP measurements, we require the value of β ≈ 1.83 thereby breaking global Weyl symmetry. We show that the general R β model can be obtained from a SUGRA construction by adding a power law ( Φ + Φ ˉ ) n term to the minimal no-scale SUGRA K?hler potential. We further show that this two-parameter power law generalization of the Starobinsky model is equivalent to generalized non-minimal curvature coupled models of the form ξ ? a R b + λ ? 4 ( 1 + γ ) and thus the power law Starobinsky model is the most economical parametrization of such models.
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机译：我们将对爱因斯坦引力的幂定律1 M 2 Rβ校正作为通货膨胀的模型。这种概括形式的有趣特征是，与Starobinsky极限β= 2的较小偏差可以将张量与标量比的值从r〜O（10？3）更改为r〜O（0.1）。我们发现，为了获得大的张量摄动r≈0.1（如BKP测量所示），我们需要β≈1.83的值，从而破坏了整体Weyl对称性。我们表明，一般的Rβ模型可以通过将幂定律（Φ+Φ）n项加到最小无尺度SUGRA Khhler势而从SUGRA构造中获得。我们进一步证明，Starobinsky模型的这种两参数幂定律推广等效于ξ？形式的广义非最小曲率耦合模型。 a R b +λ？ 4（1 +γ），因此幂定律Starobinsky模型是这种模型最经济的参数化。
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