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By Antonio Alfonso-Faus

ISBN-10: 9533076267

ISBN-13: 9789533076263

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2007c). Cosmological perturbations in warm inflationary models with viscous pressure. Phys. Rev. D, 75, 083518 del Campo, S. , (2008). Warm-Chaplygin inflationary universe model. Lett. ; Herrera, R. , (2008). Tachyon warm inflationary universe model in the weak dissipative regime. Eur. Phys. J. ; Pavón, D. R. , (2010). On the consistency of warm inflation in the presence of viscosity. JCAP, 08, 002 De Felice, A. , (2004). Baryogenesis after hyperextended inflation. Rev. ; Hu, W. , (1998). Cosmic complementarity: H(0) and Omega(m) from combining CMB experiments and redshift surveys.

6. Acknowledgments Some of the perspectives presented here in this chapter incorporates the contributions I have developed with different colleagues. Particularly, I would like to thank Ramón Herrera and Diego Pavón, with whom I have been involved in the study of warm inflation. 710/2011. 7. ; Matarrese, S. , (2003). Second-order cosmological perturbations from inflation. Nucl. Phys. R. , (2011). PLANCK early results: The power spectrum Of cosmic infrared background anisotropies. 2028 [astro-ph] Albrecht, A.

Next we introduce two N-dimensional embedded spaces. The first will be our reference manifold and is assumed to be flat; the second embedded space will be the natural manifold and will be intrinsically curved (Eshelby, 1956). Each embedded manifold has its own coordinates; for them I use the symbols ξμ (reference manifold) and x μ (natural manifold); 31 The Strained State Cosmology the μ index runs from 1 to N. , X N + n = constant (3) The index i runs from 1 to n. s (2) and (3) permit to express n of the embedding coordinates in terms of the other N on the two submanifolds.

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Aspects of Today´s Cosmology by Antonio Alfonso-Faus

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