scholarly journals TUNNELING OF MACROSCOPIC UNIVERSES

1998 ◽  
Vol 07 (02) ◽  
pp. 189-200 ◽  
Author(s):  
HEINZ-DIETER CONRADI
Keyword(s):  
Quantum Cosmology ◽  
Turning Point ◽  
Local Process ◽  
Recent Suggestion ◽  
Classical Turning Point ◽  
The Universe

The meaning of 'tunneling' in a timeless theory such as quantum cosmology is discussed. A recent suggestion of 'tunneling' of the macroscopic universe at the classical turning point is analyzed in an anisotropic and inhomogeneous toy model. This 'inhomogeneous tunneling' is a local process which cannot be interpreted as a tunneling of the universe.

Yoga and The Physics of Higher States of Consciousness

2018 ◽  
pp. 335-358
Author(s):  
Alex Hankey
Keyword(s):  
Quantum Cosmology ◽  
Sense Perception ◽  
Pure Consciousness ◽  
States Of Consciousness ◽  
Action Refinement ◽  
Higher States Of Consciousness ◽  
Modern Physics ◽  
Inner Light ◽  
The Universe

Higher states of consciousness are developed by meditation, defined by Patanjali as that which transforms focused attention into pure consciousness, the 4th state of pure consciousness - a major state in its own right, with its own physics, that of ‘experience information'. Phenomenologies of states 5 to 7 are explained from the perspective of modern physics and quantum cosmology. The role of the 5th state in life is to make possible witnessing states 1 to 3 resulting in ‘Perfection in Action'. Refinement of perception involved in the 6th State results in hearing the Cosmic Om, seeing the Inner Light, and seventh sense perception. All require special amplification processes on pathways of perception. Unity and Brahman Consciousness and their development are discussed with examples from the great sayings of the Upanishads, and similar cognitions like those of poet, Thomas Traherne. Throughout, supporting physics is given, particularly that of experience information, and its implications for Schrodinger's cat paradox and our scientific understanding of the universe as a whole.

Tomographic analysis of quantum and classical de Sitter cosmological models

2019 ◽  
Vol 28 (16) ◽  
pp. 2040009 ◽  
Author(s):  
Cosimo Stornaiolo
Keyword(s):  
Quantum Cosmology ◽  
Classical Limit ◽  
Initial Conditions ◽  
Quantum Tomography ◽  
Wave Functions ◽  
Hamiltonian Constraint ◽  
De Sitter ◽  
Quantum Universe ◽  
Tomographic Analysis ◽  
The Universe

In this work, we show the importance of introducing the quantum tomography formalism to analyze the properties of wave functions in quantum cosmology. In particular, we examine the initial conditions of the universe proposed by various authors in the context of de Sitter’s cosmology studying their classical limit and comparing it with the classical tomogram obtained from the Hamiltonian constraint in General Relativity. This comparison gives us the opportunity to find under which conditions there is a transition from the quantum universe to the classical one. A relevant result is that in these models the decay of the cosmological constant is a sufficient condition for this transition.

COSMIC TIME IN QUANTUM COSMOLOGY: INFLATION-COMPACTIFICATION AS A QUANTUM EFFECT

1993 ◽  
Vol 02 (02) ◽  
pp. 221-247 ◽  
Author(s):  
E.I. GUENDELMAN ◽  
A.B. KAGANOVICH
Keyword(s):  
Cosmological Constant ◽  
Quantum Cosmology ◽  
Quantum Effect ◽  
Cosmic Time ◽  
Expectation Values ◽  
Cosmological Singularity ◽  
Inflationary Phase ◽  
Definition Of ◽  
The Universe ◽  
Kaluza Klein

We consider 1+D-dimensional, toroidally compact Kaluza-Klein theories. In the context of the minisuperspace approach of quantum cosmology, we solve the Wheeler-DeWitt equation in the presence of a negative cosmological constant and dust. Then, it is found that the quantum effects stabilize the volume of the Universe, so that there can be an avoidance of the cosmological singularity. Although cosmic time does not appear explicitly in the Wheeler-DeWitt equation, we find that a cosmic time dependence appears for the expectation values of certain variables. This result is obtained when proper care of some subtle points concerning the definition of averages in this model is taken. The stabilization of the volume, when there is anisotropy in the evolution of the Universe (which turns out to be quantized), is consistent with another effect we find: the existence of a “quantum inflationary phase” for some dimensions and simultaneously the existence of a “quantum deflationary contraction” for the rest.

The evolutionary pictures for phantom field in loop quantum cosmology

2019 ◽  
Vol 28 (15) ◽  
pp. 1950170
Author(s):  
Kui Xiao
Keyword(s):  
Dark Matter ◽  
Quantum Cosmology ◽  
Scalar Fields ◽  
Chaplygin Gas ◽  
Loop Quantum Cosmology ◽  
Phantom Field ◽  
Dynamical Behaviors ◽  
Slow Roll ◽  
The Universe ◽  
Slow Roll Inflation

The evolutionary pictures for phantom field in loop quantum cosmology are discussed in this paper. Comparing the dynamical behaviors of the phantom field with one of the canonical scalar fields in loop quantum cosmology scenario, we found that the [Formula: see text] phase trajectories are the same, but the [Formula: see text] phase-spaces are very different, and the phantom field with considering potentials can drive neither super inflation nor slow-roll inflation in loop quantum cosmology (LQC) scenario. While the universe is filled with multiple dark fluids, to ensure that the condition [Formula: see text] does not violate, the energy density of dark matter [Formula: see text] and the equation-of-state of phantom field [Formula: see text] should satisfy the condition [Formula: see text] at the bounce point. If this constraint condition holds, the universe can enter an inflationary stage, and it is possible to unify the description of phantom field, dark matter and inflation. We introduced a toy model which has the same form of the general Chaplygin gas to unify the dark energy, dark matter and slow-roll inflation, and the slow-roll inflation of the toy model has also been discussed.

1-loop quantum cosmology: the contributions of matter fields to the wavefunction of the universe

1992 ◽  
Vol 9 (2) ◽  
pp. L27-L32 ◽  
Author(s):  
A O Barvinsky ◽  
A Y Kamenshchik ◽  
I P Karmazin ◽  
I V Mishakov
Keyword(s):  
Quantum Cosmology ◽  
Loop Quantum Cosmology ◽  
The Universe ◽  
Matter Fields

THE CHARACTERISTIC BOUNDARY RADII OF ATOMS

2005 ◽  
Vol 04 (01) ◽  
pp. 281-288 ◽  
Author(s):  
MING-BO ZHANG ◽  
DONG-XIA ZHAO ◽  
ZHONG-ZHI YANG
Keyword(s):  
Experimental Data ◽  
Ab Initio ◽  
Linear Relationship ◽  
Turning Point ◽  
Ab Initio Method ◽  
Characteristic Boundary ◽  
Classical Turning Point ◽  
Electronic Motion ◽  
Boundary Radius ◽  
Atomic Radii

The characteristic boundary radius of an atom has been defined as the distance from the classical turning point of electronic motion to the nucleus of the atom. With the ab initio method, the atomic boundary radii for elements from H through Xe are calculated. For the atoms in the same group, the radii defined in this way are of good linear relationship with the empirical radii commonly accepted, such as the van der Waals and covalent atomic radii determined by experimental data.

scholarly journals EMERGENT UNIVERSE WITH EXOTIC MATTER IN LOOP QUANTUM COSMOLOGY, DGP BRANE-WORLD AND KALUZA–KLEIN COSMOLOGY

2012 ◽  
Vol 27 (33) ◽  
pp. 1250189 ◽  
Author(s):  
PRABIR RUDRA
Keyword(s):  
Scalar Field ◽  
Quantum Cosmology ◽  
Brane World ◽  
Loop Quantum Cosmology ◽  
Tachyonic Field ◽  
Normal Matter ◽  
Emergent Scenario ◽  
Phantom Scalar ◽  
The Universe ◽  
Kaluza Klein

In this work we have investigated the emergent scenario of the Universe described by loop quantum cosmology model, DGP brane model and Kaluza–Klein cosmology. Scalar field along with barotropic fluid as normal matter is considered as the matter content of the Universe. In loop quantum cosmology it is found that the emergent scenario is realized with the imposition of some conditions on the value of the density of normal matter in case of normal and phantom scalar field. This is a surprising result indeed considering the fact that scalar field is the dominating matter component! In case of tachyonic field, emergent scenario is realized with some constraints on the value of ρ1 for both normal and phantom tachyon. In case of DGP brane-world realization of an emergent scenario is possible almost unconditionally for normal and phantom fields. Plots and table have been generated to testify this fact. In case of tachyonic field emergent scenario is realized with some constraints on [Formula: see text]. In Kaluza–Klein cosmology emergent scenario is possible only for a closed Universe in case of normal and phantom scalar field. For a tachyonic field, realization of emergent Universe is possible for all models (closed, open and flat).

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