Bubble nucleation and the Coleman-Weinberg model

Jensen, Lars Gerhard; Steinhardt, Paul J.

doi:10.1016/0550-3213(84)90021-x

Cited by 84 publications

(79 citation statements)

References 6 publications

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“…As the coupling to gravity is further increased, the Coleman-de Luccia instanton approaches the Hawking-Moss instanton-in other words, φ(σ = 0) and φ(σ = σ max ) approach the maximum of the potential [25] . For a discussion of the interpretation of but unfortunately no such instanton is known.…”

Section: Background Solutionmentioning

confidence: 99%

Open universe from inflation

1995

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We present a natural scenario for obtaining an open universe (Ω 0 < 1) through inflation. In this scenario, there are two epochs of inflationary expansion-an epoch of 'old inflation,' during which the inflaton field is stuck in a false vacuum, followed by an epoch of 'new inflation,' during which the inflaton field slowly rolls toward its true minimum. During the first epoch, inflation solves the smoothness and horizon problems. Then an open universe (with negative spatial curvature) is created by the nucleation of a single bubble. In effect Ω is instantaneously 'reset' to zero. During the subsequent 'new' inflation Ω rises toward unity. The value of Ω today is calculable in terms of the parameters of the potential, and we show that obtaining values significantly different from zero or unity (though within the range 0 < Ω < 1) does not require significant fine tuning. We compute the spectrum of density perturbations by evolving the Bunch-Davies vacuum modes across the bubble wall into its interior.

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Section: Background Solutionmentioning

confidence: 99%

Open universe from inflation

1995

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“…(3.2). In particular, if V (2) (hmax) vanishes, it gets replaced by an average around the top of the barrier [30][31][32]. Figure 3.…”

Section: Jhep07(2017)058mentioning

confidence: 99%

(Higgs) vacuum decay during inflation

Joti

Katsis

Loupas

et al. 2017

J. High Energ. Phys.

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We develop the formalism for computing gravitational corrections to vacuum decay from de Sitter space as a sub-Planckian perturbative expansion. Non-minimal coupling to gravity can be encoded in an effective potential. The Coleman bounce continuously deforms into the Hawking-Moss bounce, until they coincide for a critical value of the Hubble constant. As an application, we reconsider the decay of the electroweak Higgs vacuum during inflation. Our vacuum decay computation reproduces and improves bounds on the maximal inflationary Hubble scale previously computed through statistical techniques.

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“…The Coleman-De Luccia instanton is obtained only for potentials where this is possible (see e.g. [6]). It occurs when the value of φ 0 is chosen so that φ ′ returns to zero precisely at σ f .…”

Section: Instantonsmentioning

confidence: 99%

Open inflation without false vacua

Hawking¹,

Turok²

1998

Physics Letters B

210

272

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We show that within the framework of a definite proposal for the initial conditions for the universe, the Hartle-Hawking 'no boundary' proposal, open inflation is generic and does not require any special properties of the inflaton potential. In the simplest inflationary models, the semiclassical approximation to the Euclidean path integral and a minimal anthropic condition lead to Ω 0 ≈ 0.01. This number may be increased in models with more fields or extra dimensions.

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Bubble nucleation and the Coleman-Weinberg model

Cited by 84 publications

References 6 publications

Open universe from inflation

Open universe from inflation

(Higgs) vacuum decay during inflation

Open inflation without false vacua

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