2015/11/24 by Chao-jun Feng, Chao-Jun Feng, GE Feifei +7 · 1 citation
Physics and Astronomy · #Algorithm #Astrophysics #Baryon #Baryon acoustic oscillations #Black Holes and Theoretical Physics #Computer science #Cosmic microwave background #Cosmology #Cosmology and Gravitation Theories #Dark energy #Omega #Particle physics #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #Universe #gr-qc #hep-th
paper · pdf · doi:10.1103/physrevd.92.104038
published as Phys. Rev. D 92 (2015) 104038 · 12 pages, 5 figures
openalex publication_date 2015/11/24 · arxiv created 2015/11/25 · arxiv updated 2015/11/26 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Using the observation data of type Ia supernovae, cosmic microwave background, and baryon acoustic oscillations, we establish two concrete f(T) models with a nonminimal torsion-matter coupling extension. We study in detail the cosmological implication of our models and find they are successful in describing the observation of the Universe and its large-scale structure and evolution. In other words, these models do not change the successful aspects of the \mathrm\ensuremathΛCDM scenario under the error band of fitting values as describing the evolution history of the Universe including the radiation-dominated era, the matter-dominated era, and the present accelerating expansion. Meanwhile, the significant advantage of these models is that they could avoid the cosmological constant problem of \mathrm\ensuremathΛCDM. A joint analysis is performed by using the data of cosmic microwave background+baryon acoustic oscillations+joint light-curve analysis, which leads to \mathrm\ensuremathΩm0=0.255\ifmmode±\else\textpm\fi0.010, \mathrm\ensuremathΩb0h2=0.0221\ifmmode±\else\textpm\fi0.0003 and H0=68.54\ifmmode±\else\textpm\fi1.27 for model I and \mathrm\ensuremathΩm0=0.306\ifmmode±\else\textpm\fi0.010, \mathrm\ensuremathΩb0h2=0.0225\ifmmode±\else\textpm\fi0.0003 and H0=60.97\ifmmode±\else\textpm\fi0.44 for model II at 1\ensuremathσ confidence level. The evolution of the decelaration parameter q(a) and the effective equation of state wDE(a) are displayed. Furthermore, the resulting age of the Universe from our models is consistent with the ages of the oldest globular clusters. As for the fate of the Universe, model I and model II result in a de Sitter accelerating phase and a power-law one, respectively, even though wDE0<\ensuremath-1 makes model I look like a phantom at the present time.