An anisotropic model for evaluation of corneal elasticity in dynamic OCE (Conference Presentation)

2020 ◽  
Author(s):  
Mitchell A. Kirby ◽  
John J. Pitre ◽  
David S. Li ◽  
Tueng T. Shen ◽  
Ruikang K. Wang ◽  
...  
Keyword(s):  
Anisotropic Model

Cosmological Consequences with Randers Conformal of Finsler space

2007 ◽  
Vol 3 (2) ◽  
pp. 203-211
Author(s):  
Arunesh Pandey ◽  
R K Mishra
Keyword(s):  
Background Radiation ◽  
Finsler Space ◽  
Space Time ◽  
Anisotropic Model ◽  
Microwave Background ◽  
Microwave Background Radiation

In this paper we study an anisotropic model of space – time with Finslerian metric. The observed anisotropy of the microwave background radiation is incorporated in the Finslerian metric of space time.

scholarly journals Holographic anisotropic model for light quarks with confinement-deconfinement phase transition

2021 ◽  
Vol 2021 (6) ◽  
Author(s):  
Irina Ya. Aref’eva ◽  
Kristina Rannu ◽  
Pavel Slepov
Keyword(s):  
Phase Transition ◽  
Boundary Conditions ◽  
Chemical Potential ◽  
String Tension ◽  
Isotropic Case ◽  
Holographic Model ◽  
Anisotropic Model ◽  
Dilaton Field ◽  
Cornell Potential ◽  
Qcd Phase Diagram

Abstract We present a five-dimensional anisotropic holographic model for light quarks supported by Einstein-dilaton-two-Maxwell action. This model generalizing isotropic holographic model with light quarks is characterized by a Van der Waals-like phase transition between small and large black holes. We compare the location of the phase transition for Wilson loops with the positions of the phase transition related to the background instability and describe the QCD phase diagram in the thermodynamic plane — temperature T and chemical potential μ. The Cornell potential behavior in this anisotropic model is also studied. The asymptotics of the Cornell potential at large distances strongly depend on the parameter of anisotropy and orientation. There is also a nontrivial dependence of the Cornell potential on the boundary conditions of the dilaton field and parameter of anisotropy. With the help of the boundary conditions for the dilaton field one fits the results of the lattice calculations for the string tension as a function of temperature in isotropic case and then generalize to the anisotropic one.

A special anisotropic model of the universe (II)

1989 ◽  
Vol 21 (9) ◽  
pp. 967-970 ◽  
Author(s):  
Marcelo Samuel Berman ◽  
M. M. Som
Keyword(s):  
Anisotropic Model ◽  
The Universe

scholarly journals Field Independent Cosmic Evolution

2013 ◽  
Vol 2013 ◽  
pp. 1-12 ◽  
Author(s):  
Nayem Sk ◽  
Abhik Kumar Sanyal
Keyword(s):  
Higher Order ◽  
Noether Symmetry ◽  
Scalar Tensor Theory ◽  
Anisotropic Model ◽  
Tachyonic Field ◽  
Tensor Theory ◽  
Cosmic Evolution ◽  
Field Independent ◽  
Conserved Current ◽  
Theory Of Gravity

It has been shown earlier that Noether symmetry does not admit a form of corresponding to an action in which is coupled to scalar-tensor theory of gravity or even for pure theory of gravity taking anisotropic model into account. Here, we prove that theory of gravity does not admit Noether symmetry even if it is coupled to tachyonic field and considering a gauge in addition. To handle such a theory, a general conserved current has been constructed under a condition which decouples higher-order curvature part from the field part. This condition, in principle, solves for the scale-factor independently. Thus, cosmological evolution remains independent of the form of the chosen field, whether it is a scalar or a tachyon.

The nonlinear patterns of the cosmic anisotropy: the spatially flat perfect fluid universes.

2021 ◽  
Author(s):  
Leandro Gustavo Gomes
Keyword(s):  
Perfect Fluid ◽  
Hubble Parameter ◽  
Late Time ◽  
Algebraic Equations ◽  
Anisotropic Model ◽  
Bianchi Models ◽  
Principal Directions

Abstract In this manuscript, we investigate the patterns of the cosmological anisotropy in the spatially flat Bianchi models filled with a perfect fluid. We analyse the factor 1 + ∆R, the ratio of the Hubble parameter in the anisotropic model over its isotropic counterpart. In general, ∆R starts to deviate significantly from zero at a specific redshift zA, which depends on the type of the fluid and the value of the anisotropy magnitude. We also show that the deceleration and the jerk along the principal directions of the expansion tensor are constrained by simple algebraic equations that do not depend on the type of matter present. These characteristic patterns form a valuable framework to probe the cosmological anisotropy in the late-time universe.

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