Late-time behaviour of the tilted Bianchi type VI
                    −1/9
                    models

We calculate the tipping time of a quantum rod that has a height several times that of the edge length of its square base. We use an expression for the tipping time that has heuristic value, and gives the average time at which, upon measurement, the initially balanced rod is found to tip. We use two methods to calculate the tipping time. One method is to examine the "late time" behaviour of the quantum state of the center of mass of the rod by using an equation that has the form of the time-independent Schrödinger equation except that it involves a "complex energy." The other method uses energy resonances in the eigenstates of the Hamiltonian to determine the tipping time. We use the well-known WentzelKramersBrillouin approximation to calculate the energy eigenstates. With these methods, we obtain expressions for the tipping time that are valid for very long tipping times. PACS Nos.: 03.65.w, 03.65.Xp

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ASSISTED INFLATION

International Journal of Modern Physics A ◽

10.1142/s0217751x02011825 ◽

2002 ◽

Vol 17 (20) ◽

pp. 2755-2755

Author(s):

A. A. COLEY ◽

R. J. VAN DEN HOOGEN

Keyword(s):

Perfect Fluid ◽

Scalar Fields ◽

Cosmological Models ◽

Late Time ◽

Time Behaviour ◽

Field Curvature ◽

Scaling Solution ◽

Dynamical Properties ◽

Spatially Homogeneous ◽

Parameter Values

The dynamical properties of spatially homogeneous and isotropic cosmological models containing a barotropic perfect fluid and multiple scalar fields with independent exponential potentials is investigated. It is shown that the assisted inflationary scaling solution is the global late-time attractor for the parameter values for which the model is inflationary, even when curvature and barotropic matter are included. For all other parameter values the multi-field curvature scaling solution is the global late-time attractor (in these solutions the curvature is not dynamically negligible asymptotically). Consequently, in general all of the scalar fields in multi-field models with exponential potentials are non-negligible in late-time behaviour, contrary to what is commonly believed.

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Chaotic inflation in spatially homogeneous Bianchi type V space–time

Canadian Journal of Physics ◽

10.1139/cjp-2017-0163 ◽

2017 ◽

Vol 95 (12) ◽

pp. 1267-1270

Author(s):

Raj Bali ◽

P. Kumari

Keyword(s):

Bianchi Type ◽

Space Time ◽

Late Time ◽

De Sitter ◽

Spatially Homogeneous ◽

Inflationary Parameters ◽

Type V ◽

The Universe ◽

Anisotropic Phase ◽

Bianchi Type V

Chaotic inflationary scenario in spatially homogeneous Bianchi type V space–time following Linde (Phys. Lett. B, 129, 177 (1983). doi: 10.1016/0370-2693(83)90837-7 ) and the condition [Formula: see text] based on theory of super cooling during the cosmological phase transition proposed by Kirzhnits and Linde (Ann. Phys. 101, 195 (1976). doi: 10.1016/0003-4916(76)90279-7 ), is discussed. It has been found that the model represents anisotropic phase of the Universe in general but at late time, it isotropizes. The deceleration parameter q = −1 indicates that the model leads to de Sitter space–time. It is found that inflationary parameters, namely, slow roll parameters, and anisotropic parameters are in excellent agreement with the Planck Collaboration’s 2013 results (Astron. Astrophys. 571, A22 (2014). doi: 10.1051/0004-6361/201321569 ).

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