2013/02/28 by Xiao-Jun Yue, Jian-Yang Zhu
Physics and Astronomy · #Black Holes and Theoretical Physics #Classical mechanics #Cosmology #Cosmology and Gravitation Theories #Geometry #Hamiltonian (control theory) #Hamiltonian constraint #Holonomy #Isotropy #Loop quantum cosmology #Loop quantum gravity #Massless particle #Mathematical physics #Noncommutative and Quantum Gravity Theories #Physics #Quantum #Quantum gravity #Quantum mechanics #Scalar field #Singularity #Spacetime #Theoretical physics #gr-qc
paper · pdf · doi:10.1088/0264-9381/31/4/045008
published in Classical and Quantum Gravity 31(4), 045008 (IOP Publishing) · 16 pages, 3 figures
openalex publication_date 2014/01/22 · arxiv created 2014/01/31 · arxiv updated 2015/06/12 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The detailed formulation of loop quantum cosmology with higher order holonomy corrections has been constructed recently in the homogeneous and isotropic spacetime, yet it is important to extend the higher order holonomy corrections to include the effects of anisotropy which typically grow during the collapsing phase. In this paper we investigate the Bianchi I model in μ' scheme which truly captures the regularization of the Hamiltonian constraint. To compare with the earlier works and provide a comparison with the μ' scheme, we also investigate the μ scheme although it has many disadvantages. First we construct the effective dynamics with higher order holonomy corrections in a massless scalar field, then we extend it to the inclusion of arbitrary matter. Besides that, we also analyze the behavior of the anisotropy during the evolution of the universe. We find that in the μ' scheme, the singularity is never approached and the quantum bounce is generic as in the isotropic case, regardless of the order of the holonomy corrections. Some differences in the bouncing phase of the two schemes are also found out. It is also shown that in the two schemes the behavior of the anisotropy is not the same before and after the bounce.