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Tensor power spectrum Tensor perturbations: The second-‐order action is where The tensor power spectrum is The tensor-‐to-‐scalar ratio is These results can be readily used for concrete models of inflation. e.g., where These observables depend on the slope of the potential.
We can apply our general results to a variety of inflation models. Standard potential-‐driven inflation P ( ,X)=X V ( ) f(R) gravity Brans-‐Dicke theories Non-‐minimally coupled models Galileon inflation Field-‐derivative couplings Running kinetic couplings k-‐inflation etc… S = d 4 x g M 2 pl 2 R + P ( ,X) G 3( ,X) + L 4 + L 5 L 4 = G 4 ( ,X) R + G 4,X [( ) 2 ( µ )( µ )] L 5 = G 5 ( ,X) G µ ( µ ) 1 6 G 5,X[( ) 3 3( )( µ )( µ ) + 2( µ )( )( µ )]
Page 1 and 2: S. Tsujikawa, J. Ohashi, S.Kuro
Page 3 and 4: Old inflation (Sato, Kazanas, G
Page 5 and 6: Standard slow-‐roll inflation
Page 7 and 8: S = ⇤ d 4 x ⇥ g ⇥ R 16 G + X
Page 9 and 10: Discrimination between inflaton
Page 11 and 12: S.T., J. Ohashi, S. Kuroyanagi,
Page 13 and 14: Horndeski’s paper in 1973
Page 15: Power spectrum of curvature per
Page 19 and 20: Planck constraints on Brans-Dicke g
Page 21 and 22: Higgs inflation There are severa
Page 23 and 24: Running kinetic couplings 0.3 0.25
Page 25 and 26: f NL B R f NL ・・・nonlinear e
Page 27 and 28: Observational constraints on power-
Page 29: Potentials favored from observat

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