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Inflationary Cosmology in Modified Gravity Theories [PDF]
Symmetry, 2015 We review inflationary cosmology in modified gravity such as R2 gravity with its extensions in order to generalize the Starobinsky inflation model. In particular, we explore inflation realized by three kinds of effects: modification of gravity, the quantum anomaly, and the R2 term in loop quantum cosmology.
Kazuharu Bamba, Sergei Odintsov
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Physics Reports, 2000 I give a general review of the history of inflationary cosmology and of its present status.
Andrei Linde
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Extended Inflationary Cosmology
Physical Review Letters, 1989We present a new type of inflationary scenario based on metric formulations of gravity different from that of Einstein, e.g., a Brans-Dicke theory of gravity. Unlike previous inflation models, the inflationary phase transition can be completed via bubble nucleation.
Paul Steinhardt
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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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