Results 191 to 200 of about 2,808 (218)
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Physical Review Letters, 1991
If Peccei-Quinn (PQ) symmetry is broken after inflation, the initial axion angle is a random variable on cosmological scales; based on this fact, estimates of the relic-axion mass density give too large a value if the axion mass is less than about 10 to the -6th eV. This bound can be evaded if the universe underwent inflation after PQ-symmetry breaking
, Turner, , Wilczek
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If Peccei-Quinn (PQ) symmetry is broken after inflation, the initial axion angle is a random variable on cosmological scales; based on this fact, estimates of the relic-axion mass density give too large a value if the axion mass is less than about 10 to the -6th eV. This bound can be evaded if the universe underwent inflation after PQ-symmetry breaking
, Turner, , Wilczek
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Pramana, 1993
We review the basic features of the inflationary scenarios associated with phase transitions in the very early universe.
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We review the basic features of the inflationary scenarios associated with phase transitions in the very early universe.
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Exact inflationary cosmologies with exit
Physical Review D, 1995We find exact inflationary solutions with exit, including exact forms of the potential, by specifying the rate of expansion and using the number of e-foldings as the effective dynamical variable. These include solutions in which the potential drives nearly exponential or power-law inflation for ${\mathit{t}}_{\mathit{i}}$\ensuremath{\le}t${\mathit{t}}_{
, Maartens, , Taylor, , Roussos
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This work has been archived as it has been superseded by more recent developments in our model. In light of new insights, the concept of inflation as presented here is no longer deemed necessary. For the latest and most accurate formulation, please refer to our updated work: https://zenodo.org/records/15046630 ...
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Diffusive inflationary cosmology
Journal of Geometry and Physics, 1990The author considers the Ricci flow equation \(g'(t)=-2k Ric(g(t))+Dg(t)\) for a Riemannian metric g(t) on a compact 3-manifold, where k and D are some constants. This is related to general relativity by considering a corresponding Lorentzian metric \(^{(4)}g=-c^ 2dt^ 2+g(t).\) For metrics of this form, Einstein's vacuum field equation with ...
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Inflationary cosmology: First 30+ years
International Journal of Modern Physics D, 2015Jun'Ichi Yokoyama
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Iso-Spectral Potentials and Inflationary Quantum Cosmology
International Journal of Theoretical Physics, 2006M Sabido, J Socorro, Socorro J
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