The Effective Theory of Inflation and the Dark Matter Status in the Standard Model of the Universe - Astrophysics > Cosmology and Nongalactic AstrophysicsReportar como inadecuado




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Abstract: We present here the effective theory of inflation `a la Ginsburg-Landau inwhich the inflaton potential is a polynomial. The slow-roll expansion becomes asystematic 1-N expansion where N ~ 60. The spectral index and the ratio oftensor-scalar fluctuations are n s - 1 = O1-N, r = O1-N while the runningturns to be d n s-d \ln k = O1-N^2 and can be neglected. The energy scale ofinflation M ~ 0.7 10^{16} GeV is completely determined by the amplitude of thescalar adiabatic fluctuations. A complete analytic study plus the Monte CarloMarkov Chains MCMC analysis of the available CMB+LSS data showed: a thespontaneous breaking of the phi -> - phi symmetry of the inflaton potential.b a lower bound for r: r > 0.023 95% CL and r > 0.046 68% CL. c Thepreferred inflation potential is a double well, even function of the field witha moderate quartic coupling yielding as most probable values: n s = 0.964, r =0.051. This value for r is within reach of forthcoming CMB observations. Weinvestigate the DM properties using cosmological theory and the galaxyobservations. Our DM analysis is independent of the particle physics model forDM and it is based on the DM phase-space density rho {DM}-sigma^3 {DM}. Wederive explicit formulas for the DM particle mass m and for the number ofultrarelativistic degrees of freedom g d hence the temperature at decoupling.We find that m turns to be at the keV scale. The keV scale DM isnon-relativistic during structure formation, reproduces the small and largescale structure but it cannot be responsible of the e^+ and pbar excess incosmic rays which can be explained by astrophysical mechanisms Abridged.



Autor: H. J. de Vega

Fuente: https://arxiv.org/



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