Dynamics of the Bianchi IX model near the cosmological singularity

2013 ◽  
Author(s):  
Ewa Czuchry
Keyword(s):  
Cosmological Singularity ◽  
Bianchi Ix

Particle production near the cosmological singularity

1980 ◽  
Vol 42 (1) ◽  
pp. 14-22
Author(s):  
O. Yu. Karmanov ◽  
M. B. Menskii
Keyword(s):  
Particle Production ◽  
Cosmological Singularity

scholarly journals Affine quantization and the initial cosmological singularity

2013 ◽  
Vol 101 (1) ◽  
pp. 10001 ◽  
Author(s):  
M. Fanuel ◽  
S. Zonetti
Keyword(s):  
Cosmological Singularity

On the Influence of Noise on the Bianchi ix and viii Cosmological Models

1998 ◽  
Vol 9 (11) ◽  
pp. 1813-1825 ◽  
Author(s):  
John Argyris ◽  
Ioannis Andreadis ◽  
Corneliu Ciubotariu
Keyword(s):  
Cosmological Models ◽  
Bianchi Ix ◽  
Influence Of Noise

Cosmological singularity at the Planck scale

1992 ◽  
Vol 33 (11) ◽  
pp. 3954-3956
Author(s):  
Anne Magnon
Keyword(s):  
Planck Scale ◽  
Cosmological Singularity

scholarly journals The Bianchi IX Attractor

2001 ◽  
Vol 2 (3) ◽  
pp. 405-500 ◽  
Author(s):  
H. Ringström
Keyword(s):  
Bianchi Ix

scholarly journals Bianchi IX model: Reducing phase space

2013 ◽  
Vol 87 (8) ◽  
Author(s):  
Ewa Czuchry ◽  
Włodzimierz Piechocki
Keyword(s):  
Phase Space ◽  
Bianchi Ix

scholarly journals REFLECTIONS ON THE HYPERBOLIC PLANE

2013 ◽  
Vol 22 (14) ◽  
pp. 1350085
Author(s):  
ORCHIDEA MARIA LECIAN
Keyword(s):  
Physical Interpretation ◽  
Hyperbolic Plane ◽  
Einstein Equations ◽  
Billiard Table ◽  
Billiard Ball ◽  
Cosmological Singularity ◽  
Triangular Domain ◽  
Quantum Properties ◽  
Poincaré Return Map

The most general solution to the Einstein equations in 4 = 3 + 1 dimensions in the asymptotic limit close to the cosmological singularity under the BKL (Belinskii–Khalatnikov–Lifshitz) hypothesis can be visualized by the behavior of a billiard ball in a triangular domain on the Upper Poincaré Half Plane (UPHP). The billiard system (named "big billiard") can be schematized by dividing the successions of trajectories according to Poincaré return map on the sides of the billiard table, according to the paradigms implemented by the BKL investigation and by the CB–LKSKS (Chernoff–Barrow–Lifshitz–Khalatnikov–Sinai–Khanin–Shchur) one. Different maps are obtained, according to different symmetry-quotienting mechanisms used to analyze the dynamics. In the inhomogeneous case, new structures have been uncovered, such that, in this framework, the billiard table (named "small billiard") consists of 1/6 of the previous one. The connections between the symmetry-quotienting mechanisms are further investigated on the UPHP. The relation between the complete billiard and the small billiard are also further explained according to the role of Weyl reflections. The quantum properties of the system are sketched as well, and the physical interpretation of the wave function is further developed. In particular, a physical interpretation for the symmetry-quotienting maps is proposed.

scholarly journals Motives and periods in Bianchi IX gravity models

2018 ◽  
Vol 108 (12) ◽  
pp. 2729-2747 ◽  
Author(s):  
Wentao Fan ◽  
Farzad Fathizadeh ◽  
Matilde Marcolli
Keyword(s):  
Gravity Models ◽  
Bianchi Ix

scholarly journals Cosmological singularities in interacting dark energy models with an ω(q) parametrization

2019 ◽  
Vol 28 (01) ◽  
pp. 1950019 ◽  
Author(s):  
Emilio Elizalde ◽  
Martiros Khurshudyan ◽  
Shin’ichi Nojiri
Keyword(s):  
Dark Energy ◽  
Energy Budget ◽  
Deceleration Parameter ◽  
Finite Time ◽  
Numerical Solutions ◽  
Unstable State ◽  
Stable Node ◽  
Type I ◽  
Cosmological Singularity ◽  
Time Future

Future singularities arising in a family of models for the expanding universe, characterized by sharing a convenient parametrization of the energy budget in terms of the deceleration parameter, are classified. Finite-time future singularities are known to appear in many cosmological scenarios, in particular, in the presence of viscosity or nongravitational interactions, the last being known to be able to suppress or just change in some cases the type of the cosmological singularity. Here, a family of models with a parametrization of the energy budget in terms of the deceleration parameter are studied in the light of Gaussian processes using reconstructed data from [Formula: see text]-value [Formula: see text] datasets. Eventually, the form of the possible nongravitational interaction between dark energy and dark matter is constructed from these smoothed [Formula: see text] data. Using phase space analysis, it is shown that a noninteracting model with dark energy [Formula: see text] ([Formula: see text] being the deceleration parameter) may evolve, after starting from a matter-dominated unstable state, into a de Sitter universe (the solution being in fact a stable node). Moreover, for a model with interaction term [Formula: see text] ([Formula: see text] is a parameter and [Formula: see text], the Hubble constant) three stable critical points are obtained, which may have important astrophysical implications. In addition, part of the paper is devoted to a general discussion of the finite-time future singularities obtained from direct numerical integration of the field equations, since they appear in many cosmological scenarios and could be useful for future extended studies of the models here introduced. Numerical solutions for the new models, produce finite-time future singularities of Type I or Type III, or an [Formula: see text]-singularity, provided general relativity describes the background dynamics.

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