Warm anisotropic inflation with bulk viscous pressure in intermediate era |
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| Institution: | 1. Bogoliubov Laboratory of Theoretical Physics, Joint Institute for Nuclear Research, Dubna 141980, Moscow region, Russia;2. Fachbereich Physik, Universität Wuppertal, D-42097 Wuppertal, Germany;3. Institut für Theoretische Physik, Universität Regensburg, D-93040 Regensburg, Germany;1. Physics Department and Biruni Observatory, College of Sciences, Shiraz University, Shiraz 71454, Iran;2. Research Institute for Astronomy and Astrophysics of Maragha (RIAAM), P.O. Box 55134-441, Maragha, Iran;1. Information Media Center, Hiroshima University, Higashi-Hiroshima, 739-8521, Japan;2. Department of Physics, Hiroshima University, Higashi-Hiroshima, 739-8526, Japan;3. Instituto de Ciencias del Espacio (ICE/CSIC) and Institut de Estudis Espacials de Catalunya (IEEC), Campus UAB, Carrer de Can Magrans, s/n 08193 Cerdanyola del Vallés (Barcelona), Spain;4. Institució Catalana de Recerca i Estudis Avançats (ICREA), Barcelona, Spain;5. National Research Tomsk State University, 634050 Tomsk, Russia;6. Tomsk State Pedagogical University, 634061 Tomsk, Russia;7. Inst. of Physics, Kazan Federal University, 420008 Kazan, Russia;1. Quantum Physics and Magnetism Team, LPMC, Faculty of Science Ben M''sik, Casablanca Hassan II University, Morocco;2. Lab of High Energy Physics, Modeling and Simulations, Faculty of Science, University Mohammed V-Agdal, Rabat, Morocco;3. Department of Mathematics, S. P. M. Science and Gilani Arts Commerce College, Ghatanji, Yavatmal, Maharashtra-445301, India |
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| Abstract: | The aim of this paper is to study the warm inflation during intermediate era in the framework of locally rotationally symmetric Bianchi type I universe model. We assume that the universe is composed of inflaton and imperfect fluid having radiation and bulk viscous pressure. To this end, dynamical equations (first model field equation and energy conservation equations) under slow-roll approximation and in high dissipative regime are constructed. A necessary condition is developed for the realization of this anisotropic model. We assume both dissipation and bulk viscous coefficients variable as well as constant. We evaluate entropy density, scalar (tensor) power spectra, their corresponding spectral indices, tensor–scalar ratio and running of spectral index in terms of inflaton. These cosmological parameters are constrained using recent Planck and WMAP7 probe. |
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| Keywords: | Warm inflation Slow-roll approximation Viscous pressure |
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