Slow-roll reconstruction for running spectral index

Details Slow-roll reconstruction for running spectral index Slow-roll reconstruction for running spectral index

2006-10-31

arxiv.org/abs/astro-ph/0610924v2

Phys.Rev.D76:043505,2007

Astronomy and Astrophysics

Astrophysics

18 pages, 7 figures; refs added, version for publication in PRD

Scientific paper

10.1103/PhysRevD.76.043505

We not only reconstruct the slow-roll parameters for fit to the running spectral index from WMAP three-year data in the usual slow-roll inflation model and noncommutative inflation model, but also investigate the evolution of these slow-roll parameters. Requiring slow-roll inflation lasts more than 20 e-folds after CMB scales leave the horizon suggests that the potential at the last stage of inflation takes the form $V(\phi)=V_0(1+{\eta_c\over 2}{(\phi-\phi_c)^2\over M_p^2})$, where $\eta_c$ is a constant. A natural mechanism to end inflation at $\phi=\phi_c$ is hybrid type inflation.

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