Recent progress in inflationary cosmology

Linde, Andrei

doi:10.1007/3-540-60024-8_130

Cited by 7 publications

(7 citation statements)

References 37 publications

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“…One may try to find a stationary solution of equations ( 18), (19), assuming that ∂Pc(φ,t|φ0) ∂t = 0. The simplest stationary solution (subexponential factors being omitted) would be [10,44,23]…”

Section: Wave Function Of the Universe And Stochastic Approach To Inf...mentioning

confidence: 99%

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Quantum creation of an open inflationary universe

1998

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We discuss a dramatic difference between the description of the quantum creation of an open universe using the Hartle-Hawking wave function and the tunneling wave function. Recently Hawking and Turok have found that the Hartle-Hawking wave function leads to a universe with Ω = 0.01, which is much smaller that the observed value of Ω. Galaxies in such a universe would be 10 10 8 light years away from each other, so the universe would be practically structureless. We argue that the Hartle-Hawking wave function does not describe the probability of creation of the universe. If one uses the tunneling wave function for the description of creation of the universe, then in most inflationary models the universe should have Ω = 1, which agrees with the standard expectation that inflation makes the universe flat. The same result can be obtained in the theory of a selfreproducing inflationary universe, independently of the issue of initial conditions. However, there exist some models where Ω may take any value, from Ω > 1 to Ω ≪ 1.

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Section: Wave Function Of the Universe And Stochastic Approach To Inf...mentioning

confidence: 99%

“…Thus, in this scenario one does not encounter any problems in creating an open universe from nothing. In fact one does not create a single open universe but infinitely many of them, with different values of Ω in each of the universes [19].…”

Section: Introductionmentioning

confidence: 99%

Quantum creation of an open inflationary universe

1998

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“…One may consider a purely classical evolution of an inflationary universe in the false vacuum and a subsequent creation of inflating open universes by tunneling to the true vacuum [1][2][3]. Alternatively, one may consider the quantum creation from nothing of a closed inflationary universe, which later decays into an infinite number of open universes by the process described above [4,5]. In all such models, it is necessary to assume a potential with a false vacuum.…”

Section: Introductionmentioning

confidence: 99%

Quantum creation of a universe with Ω≠1: Singular and nonsingular instantons

Bousso

Linde

1998

Phys. Rev. D

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We propose two new classes of instantons which describe the tunneling and/or quantum creation of closed and open universes. The instantons leading to an open universe can be considered as generalizations of the Coleman-De Luccia solution. They are nonsingular, unlike the instantons recently studied by Hawking and Turok, whose prescription has the problem that the singularity is located on the hypersurface connecting to the Lorentzian region, which makes it difficult to remove. We argue that such singularities are harmless if they are located purely in the Euclidean region. We thus obtain new singular instantons leading to a closed universe; unlike the usual regular instantons used for this purpose, they do not require complex initial conditions. The singularity gives a boundary contribution to the action which is small for the instantons leading to sufficient inflation, but changes the sign of the action for small corresponding to short periods of inflation.

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“…Where µ, ν = 0, ..., 3. As our main interest is bosonic configurations that preserve some supersymmetry, the stress tensor can be simplified by considering the vanishing of the supersymmetric variations (11,12); satisfying the BPS condition on the brane. This gives…”

Section: Five Dimensional N = 2 Supergravitymentioning

confidence: 99%

“…There are many proposed models of 'brane-cosmology' in which the Universe is considered as a 3-brane (supersymmetric or non-supersymmetric) embedded in a higher dimensional spacetime [10]. Some of these models explain inflation based on the existence of a scalar field in the early Universe called the 'inflaton' [11]. Other models focus on the late-time acceleration of the Universe [12].…”

Section: Introductionmentioning

confidence: 99%

Interpreting the cosmic history of the Universe through five-dimensional supergravity

Emam

Salem

2023

Class. Quantum Grav.

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Through modeling the universe as a symplectic 3-brane embedded in the bulk of N = 2 five-dimensional ungauged supergravity theory, the entire evolution of the universe can be interpreted from inflation to late-time acceleration without introducing an inflaton nor a cosmological constant. The time dependence of the brane is strongly correlated to the complex structure mod- uli of the underlying Calabi-Yau submanifold and the bulk effects. The solutions to the field equations are found by exploiting the theory’s symplectic structure where the time evolution is similar to our universe according to the latest data of the Planck mission. Our results present a new explanation for the nature of dark energy mainly based on the topology of the subspace and the existence of a fifth extra dimension.

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Recent progress in inflationary cosmology

Cited by 7 publications

References 37 publications

Quantum creation of an open inflationary universe

Quantum creation of an open inflationary universe

Quantum creation of a universe with Ω≠1: Singular and nonsingular instantons

Interpreting the cosmic history of the Universe through five-dimensional supergravity

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