Comment on the Bianchi type-I solution with conformally invariant scalar field

1985 ◽  
Vol 85 (2) ◽  
pp. 161-164
Author(s):  
D. Lorentz-Petzold
Keyword(s):  
Scalar Field ◽  
Bianchi Type ◽  
Type I ◽  
Bianchi Type I ◽  
Conformally Invariant ◽  
Invariant Scalar

Bianchi type-I models with conformally invariant scalar field

1983 ◽  
Vol 27 (10) ◽  
pp. 2282-2284 ◽  
Author(s):  
A. J. Accioly ◽  
A. N. Vaidya ◽  
M. M. Som
Keyword(s):  
Scalar Field ◽  
Bianchi Type ◽  
Type I ◽  
Bianchi Type I ◽  
Conformally Invariant ◽  
Invariant Scalar

scholarly journals Decoupling of the general scalar field mode and the solution space for Bianchi type I and V cosmologies coupled to perfect fluid sources

2006 ◽  
Vol 47 (4) ◽  
pp. 042505 ◽  
Author(s):  
T. Christodoulakis ◽  
Th. Grammenos ◽  
Ch. Helias ◽  
P. G. Kevrekidis ◽  
A. Spanou
Keyword(s):  
Scalar Field ◽  
Perfect Fluid ◽  
Bianchi Type ◽  
Solution Space ◽  
Type I ◽  
Field Mode ◽  
Bianchi Type I ◽  
General Scalar ◽  
Fluid Sources

scholarly journals Intermediate inflation with non-canonical scalar field in the low anisotropy Universe

2019 ◽  
Vol 34 (33) ◽  
pp. 1950272
Author(s):  
Mahdieh Naderi ◽  
Ali Aghamohammadi ◽  
Abdollah Refaei ◽  
Haidar Sheikhahmadi
Keyword(s):  
Scalar Field ◽  
Bianchi Type ◽  
Type I ◽  
Spectral Indices ◽  
Common Procedure ◽  
Bianchi Type I ◽  
Good Consistency ◽  
Bianchi Type I Universe ◽  
Homogeneous Universe ◽  
Canonical Scalar Field

The behavior of a non-canonical scalar field within an anisotropic Bianchi type I, spatially homogeneous Universe in the framework of the intermediate inflation will be studied. It will be examined on the condition that both the anisotropy and non-canonical sources come together if there is any improvement in compatibility with the observational data originated from Planck 2015. Based on this investigation, it can be observed that automatically a steep potential which can manage inflation in a better way will be obtained. Additionally, as a common procedure for an inflationary study, we shall try to calculate the related inflationary observables such as the amplitude of the scalar perturbations, scalar and tensor spectral indices, tensor-to-scalar ratio, the running spectral index and the number of e-folds. As an exciting part of our results, we will find that our model has a good consistency compared to data resulting from CMB and different Planck results. To justify our claims, the well-known canonical inflationary scenario in an anisotropic Bianchi type I Universe will also be evaluated.

Chameleon scalar field in LRS Bianchi type I cosmological model

2016 ◽  
Vol 22 (1) ◽  
pp. 54-63 ◽  
Author(s):  
R. Chaubey ◽  
Ashutosh Singh ◽  
Rakesh Raushan
Keyword(s):  
Scalar Field ◽  
Cosmological Model ◽  
Bianchi Type ◽  
Type I ◽  
Bianchi Type I

Bianchi type – I dark energy cosmological model coupled with a massive scalar field

New Astronomy ◽  
2021 ◽  
pp. 101733
Author(s):  
M.P.V.V. Bhaskara Rao ◽  
R.L. Naidu ◽  
Y. Aditya ◽  
D.R.K. Reddy
Keyword(s):  
Dark Energy ◽  
Scalar Field ◽  
Cosmological Model ◽  
Bianchi Type ◽  
Type I ◽  
Massive Scalar ◽  
Massive Scalar Field ◽  
Bianchi Type I

scholarly journals CREATION OF THE NONCONFORMAL SCALAR PARTICLES IN NONSTATIONARY METRIC

2002 ◽  
Vol 17 (06n07) ◽  
pp. 1041-1044 ◽  
Author(s):  
YU. V. PAVLOV
Keyword(s):  
Wave Equation ◽  
Scalar Field ◽  
Bianchi Type ◽  
Dimensional Space ◽  
Type I ◽  
Bianchi Type I ◽  
Scalar Particles ◽  
Oscillator Frequency ◽  
Dimensional Space Time ◽  
Anisotropic Spaces

The nonconformal scalar field is considered in N-dimensional space-time with metric which includes, in particular, the cases of nonhomogeneous spaces and anisotropic spaces of Bianchi type-I. The modified Hamiltonian is constructed. Under the diagonalization of it the energy of quasiparticles is equal to the oscillator frequency of the wave equation. The density of particles created by nonstationary metric is investigated. It is shown that the densities of conformal and nonconformal particles created in Friedmann radiative-dominant universe coincide.

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