A new inflaton model beginning near the Planck epoch

Autor(es)

Reuven Opher ^[1] ; Ana Pelinson ^[2]

Afiliação do(s) autor(es)

^[1] Universidade de São Paulo. IAG. Departamento de Astronomia

^[2] Universidade de São Paulo. IAG. Departamento de Astronomia

• Tipo de documento: Artigo Científico
• Fonte: Brazilian Journal of Physics; v. 36, p. 566-569, 2006-06-00.

Resumo

The Starobinsky model predicts a primordial inflation period without the presence of an inflaton field. The modified version of this model predicts a simple time dependence for the Hubble parameter H(t), which decreases slowly between the Planck epoch and the end of the inflation, H(t) = M Pl -betaM²Pl t, where beta is a dimensionless constant to be adjusted from observations. We investigate an inflaton model which has the same time dependence for H(t). A reverse engineered inflaton potential for the time dependence of H is derived. Normalization of the derived inflaton potential is determined by the condition that the observed density fluctuations, <FONT FACE=Symbol>dr</FONT>/<FONT FACE=Symbol>r »</FONT> 10-5, are created at ~ 60 e-folds before the end of inflation. The derived potential indicates an energy (mass) scale, Mend ~ 10(13) GeV, at the end of inflation. Using the slow roll parameters, which are obtained from this potential, we calculate the spectral index for the scalar modes nS and the relative amplitude of the tensor to scalar modes r. A tensor contribution, r ~ 0.13, and an approximately Harrison-Zeldovich density perturbation spectrum, nS ~ 0.95, are predicted. (AU)

• Processo FAPESP: 03/04516-0 - Confrontando as previsões da teoria de inflação baseado nos efeitos de vácuo com as observações
• Beneficiário: Ana das Mercês Pelinson
• Modalidade de apoio: Bolsas no Brasil - Pós-Doutorado
• Processo FAPESP: 00/06770-2 - Radiação cósmica de fundo em microondas e formação de estruturas no universo
• Beneficiário: Reuven Opher
• Modalidade de apoio: Auxílio à Pesquisa - Temático