Bianchi-type cosmological models in Lyra’s geometry with constant deceleration parameter

1993 ◽  
Vol 108 (5) ◽  
pp. 541-558
Author(s):  
T. Singh ◽  
Anil K. Agrawal
Keyword(s):  
Deceleration Parameter ◽  
Bianchi Type ◽  
Cosmological Models ◽  
Constant Deceleration Parameter ◽  
Lyra’S Geometry

scholarly journals LRS BIANCHI TYPE-I COSMOLOGICAL MODELS IN BARBER'S SECOND SELF CREATION THEORY

2002 ◽  
Vol 11 (08) ◽  
pp. 1195-1207 ◽  
Author(s):  
ANIRUDH PRADHAN ◽  
ANIL KUMAR VISHWAKARMA
Keyword(s):  
Physical Properties ◽  
Exact Solutions ◽  
Perfect Fluid ◽  
Deceleration Parameter ◽  
Bianchi Type ◽  
Cosmological Models ◽  
Type I ◽  
Fluid Source ◽  
Bianchi Type I ◽  
Radiation Universe

Barber's second self creation theory with perfect fluid source for an LRS Bianchi type-I metric is considered using deceleration parameter to be constant where the metric potentials are taken as functions of x and t. In particular, some exact solutions have also been obtained for the vacuum universe, Zel'dovich universe and radiation universe. Some physical properties of the models are also discussed.

scholarly journals Anisotropic magnetized holographic Ricci dark energy cosmological models

2017 ◽  
Vol 95 (4) ◽  
pp. 381-392 ◽  
Author(s):  
M. Vijaya Santhi ◽  
V.U.M. Rao ◽  
Y. Aditya
Keyword(s):  
General Relativity ◽  
Dark Energy ◽  
Deceleration Parameter ◽  
Bianchi Type ◽  
Cosmological Models ◽  
Field Equations ◽  
Ricci Dark Energy ◽  
Theor Phys ◽  
Linearly Varying Deceleration Parameter ◽  
Spatially Homogeneous

In this paper, we have considered spatially homogeneous and anisotropic Bianchi type-III space–time filled with matter and anisotropic modified holographic Ricci dark energy in general relativity. We have solved Einstein’s field equations using the following possibilities: (i) hybrid expansion law proposed by Akarsu et al. (JCAP, 01, 022 (2014)); (ii) a varying deceleration parameter considered by Mishra et al. (Int. J. Theor. Phys. 52, 2546 (2013)); and (iii) a linearly varying deceleration parameter given by Akarsu and Dereli (Int. J. Theor. Phys. 51, 612 (2012)). We have presented the cosmological models in each of the preceding cases and studied their evolutions. We have also discussed physical and kinematical properties of the models.

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