scholarly journals QUANTIZATION OF THE BIANCHI TYPE IX MODEL IN N=1 SUPERGRAVITY IN THE PRESENCE OF SUPERMATTER

1996 ◽  
Vol 11 (10) ◽  
pp. 1763-1795 ◽  
Author(s):  
P.V. MONIZ
Keyword(s):  
Wave Function ◽  
Scalar Field ◽  
General Theory ◽  
Bianchi Type ◽  
Two Dimensional ◽  
Kahler Geometry ◽  
Complex Scalar ◽  
Analytical Potential ◽  
Complex Scalar Field ◽  
The Universe

The general theory of N=1 supergravity with supermatter is applied to a Bianchi type IX diagonal model. The supermatter is constituted by a complex scalar field and its [Formula: see text] fermionic partners. The Kähler geometry is chosen to be a two-dimensional flat one. The Lorentz-invariant ansatz for the wave function of the universe is taken to be as simple as possible in order to obtain new solutions. The set of differential equations derived from the quantum constraints are analyzed in two different cases: if the supermatter terms include an analytical potential or not. In the latter the wave function is found to have a simple form.

scholarly journals Complex Inflaton Field in Quantum Cosmology

1997 ◽  
Vol 06 (06) ◽  
pp. 649-671 ◽  
Author(s):  
A. Yu. Kamenshchik ◽  
I. M. Khalatnikov ◽  
A. V. Toporensky
Keyword(s):  
Scalar Field ◽  
Cosmological Model ◽  
Equations Of Motion ◽  
Inflationary Cosmology ◽  
Complex Scalar ◽  
Inflaton Field ◽  
Absolute Value ◽  
Forbidden Regions ◽  
Complex Scalar Field ◽  
The Universe

We investigate the cosmological model with the complex scalar self-interacting inflaton field non-minimally coupled to gravity. The different geometries of the Euclidean classically forbidden regions are represented. The instanton solutions of the corresponding Euclidean equations of motion are found by numerical calculations supplemented by the qualitative analysis of Lorentzian and Euclidean trajectories. The applications of these solutions to the no-boundary and tunneling proposals for the wave function of the Universe are studied. Possible interpretation of obtained results and their connection with inflationary cosmology is discussed. The restrictions on the possible values of the new quasifundamental constant of the theory — non-zero classical charge — are obtained. The equations of motion for the generalized cosmological model with complex scalar field are written down and investigated. The conditions of the existence of instanton solutions corresponding to permanent values of an absolute value of scalar field are obtained.

scholarly journals ON THE TRANSITION FROM COMPLEX TO REAL SCALAR FIELDS IN MODERN COSMOLOGY

2011 ◽  
Vol 08 (08) ◽  
pp. 1815-1832 ◽  
Author(s):  
GIAMPIERO ESPOSITO ◽  
RAJU ROYCHOWDHURY ◽  
CLAUDIO RUBANO ◽  
PAOLO SCUDELLARO
Keyword(s):  
Dark Energy ◽  
Scalar Field ◽  
Scalar Fields ◽  
Complex Nature ◽  
Complex Scalar ◽  
Real Scalar ◽  
Symmetry Approach ◽  
Modern Cosmology ◽  
Complex Scalar Field ◽  
The Universe

We study some problems arising from the introduction of a complex scalar field in cosmology, modeling its possible behaviors in both the inflationary and dark energy stages of the universe. Such examples contribute to show that, while the complex nature of the scalar field can be indeed important during inflation, it loses its meaning in the later dark-energy dominated era of cosmology, when the phase of the complex field is practically constant, and there is indeed a transition from complex to real scalar field. In our considerations, the Noether symmetry approach turns out to be a useful tool once again. We arrive eventually at a potential containing the sixth and fourth powers of the scalar field, and the resulting semiclassical quantum cosmology is studied to gain a better understanding of the inflationary stage.

scholarly journals Wave Function for the Reissner–Nordström Black Hole

1997 ◽  
Vol 12 (20) ◽  
pp. 1491-1505 ◽  
Author(s):  
P. V. Moniz
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Wave Function ◽  
Scalar Field ◽  
Hawking Radiation ◽  
Apparent Horizon ◽  
Complex Scalar ◽  
Charge Rate ◽  
Quantum Behavior ◽  
Complex Scalar Field

We study the quantum behavior of Reissner–Nordström (RN) black holes interacting with a complex scalar field. A Maxwell field is also present. Our analysis is based on M. Pollock's1 method and is characterized by solving a Wheeler–DeWitt equation in the proximity of an apparent horizon of the RN space–time. Subsequently, we obtain a wave function Ψ RN [M,Q] representing the RN black hole when its charge, |Q|, is small in comparison with its mass, M. We then compare quantum-mechanically the cases of (i) Q=0 and (ii) M≥|Q|≠0. A special emphasis is given to the evolution of the mass-charge rate affected by Hawking radiation.

scholarly journals QUANTUM REMNANT AS DARK ENERGY AND DARK MATTER

2011 ◽  
Vol 01 ◽  
pp. 277-284
Author(s):  
SANG PYO KIM ◽  
SEOKTAE KOH
Keyword(s):  
Dark Matter ◽  
Dark Energy ◽  
Scalar Field ◽  
Uncertainty Principle ◽  
Dark Energy Model ◽  
Quantum Fluctuations ◽  
Complex Scalar ◽  
Linear Perturbations ◽  
Complex Scalar Field ◽  
The Universe

We study the quantum remnant of a scalar field protected by the uncertainty principle. The quantum remnant that survived the later stage of evolution of the universe may provide dark energy and dark matter depending on the potential. Though the quantum remnant shares some useful property of complex scalar field (spintessence) dark energy model, quantum fluctuations are still unstable to the linear perturbations for V ~ ϕq with q < 1 as in the spintessence model.

scholarly journals INFLATIONARY SOLUTIONS WITH A FIVE-DIMENSIONAL COMPLEX SCALAR FIELD

2006 ◽  
Vol 21 (05) ◽  
pp. 409-419
Author(s):  
J. J. VAN DER BIJ ◽  
EUGEN RADU
Keyword(s):  
Scalar Field ◽  
Field Potential ◽  
Accelerated Expansion ◽  
Complex Scalar ◽  
Dimensional Spacetime ◽  
Klein Gordon ◽  
Expansion Of The Universe ◽  
Complex Scalar Field ◽  
New Feature ◽  
The Universe

We discuss inflationary solutions of the coupled Einstein–Klein–Gordon equations for a complex field in a five-dimensional spacetime with a compact x5 dimension. As a new feature, the scalar field contains a dependence on the extra dimension of the form exp (imx5), corresponding to Kaluza–Klein excited modes. In a four-dimensional picture, a nonzero m implies the presence of a new term in the scalar field potential. An interesting feature of these solutions is the possible existence of several periods of oscillation of the scalar field around the equilibrium value at the minimum of the potential. These oscillations lead to cosmological periods of accelerated expansion of the universe.

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