1999/06/28 by Shinji Tsujikawa, S. Tsujikawa, K. Maeda +3 · 1 citation
Mathematics · Physics and Astronomy · #Approx #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #Curvature #Geometry #Inflation (cosmology) #Mathematical physics #Mathematics #Particle physics #Physics #Scalar field #Solar and Space Plasma Dynamics #Theoretical physics #astro-ph #gr-qc #hep-ph #hep-th
paper · pdf · doi:10.1103/physrevd.60.123505
published as Phys.Rev.D60:123505,1999 · 31pages, 12figures
arxiv created 1999/06/28 · openalex publication_date 1999/11/15 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
In higher-curvature inflation models (R+\ensuremathαnRn), we study a parametric preheating of a scalar field \ensuremathχ coupled nonminimally to a spacetime curvature R(\ensuremathξR\ensuremathχ2). In the case of the R2-inflation model, efficient preheating becomes possible for rather small values of \ensuremathξ, i.e., |\ensuremathξ|\ensuremath\lesssim several. Although the maximal fluctuation √〈\ensuremathχ2〉max\ensuremath≈2\ifmmode×\else\texttimes\fi1017GeV for \ensuremathξ\ensuremath≈\ensuremath-4 is almost the same as the chaotic inflation model with a nonminimally coupled \ensuremathχ field, the growth rate of the fluctuation becomes much larger and efficient preheating is realized. We also investigate preheating for the R4 model and find that the maximal fluctuation is √〈\ensuremathχ2〉max\ensuremath≈8\ifmmode×\else\texttimes\fi1016GeV for \ensuremathξ\ensuremath≈\ensuremath-35.