2016/07/31 by Jaume de Haro, Jaume Amorós, Supriya Pan · 2 citations
Physics and Astronomy · #Cosmology #Cosmology and Gravitation Theories #Dark Matter and Cosmic Phenomena #Dark energy #Inflation (cosmology) #Invertible matrix #Mathematical physics #Physics #Planck #Quantum mechanics #Quintessence #Solar and Space Plasma Dynamics #Spectral index #Spectral line #Theoretical physics #gr-qc
paper · pdf · doi:10.1103/physrevd.94.064060
published as Phys. Rev. D 94, 064060 (2016) · Version accepted for publication in PRD
arxiv created 2016/09/12 · openalex publication_date 2016/09/21 · arxiv updated 2016/09/28 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The present work is a sequel of our previous work [Phys. Rev. D 93, 084018 (2016)] which depicted a simple version of an inflationary quintessential model whose inflationary stage was described by a Higgs-type potential and the quintessential phase was responsible due to an exponential potential. Additionally, the model predicted a nonsingular universe in past which was geodesically past incomplete. Further, it was also found that the model is in agreement with the Planck 2013 data when running is allowed. But, this model provides a theoretical value of the running which is far smaller than the central value of the best fit in ns, r, \ensuremathαs\ensuremath≡dns/dlnk parameter space where ns, r, \ensuremathαs respectively denote the spectral index, tensor-to-scalar ratio and the running of the spectral index associated with any inflationary model, and consequently to analyze the viability of the model one has to focus in the two-dimensional marginalized confidence level in the allowed domain of the plane (ns,r) without taking into account the running. Unfortunately, such analysis shows that this model does not pass this test. However, in this sequel we propose a family of models runs by a single parameter \ensuremathα\ensuremath∈[0,1] which proposes another ``inflationary quintessential model'' where the inflation and the quintessence regimes are respectively described by a power law potential and a cosmological constant. The model is also nonsingular although geodesically past incomplete as in the cited model. Moreover, the present one is found to be more simple compared to the previous model and it is in excellent agreement with the observational data. In fact, we note that, unlike the previous model, a large number of the models of this family with \ensuremathα\ensuremath∈[0,(1)/(2)) match with both Planck 2013 and Planck 2015 data without allowing the running. Thus, the properties in the current family of models compared to its past companion justify its need for a better cosmological model with the successive improvement of the observational data.