Quantum tunneling in flux compactifications

Blanco-Pillado, José J.; Schwartz-Perlov, Delia; Vilenkin, Alexander

doi:10.1088/1475-7516/2009/12/006

Cited by 67 publications

(130 citation statements)

References 48 publications

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“…Therefore the 'nothing' inside the bubble of nothing should be understood as the limit of anti-de Sitter space as the curvature length approaches zero. 9 We then applied this understanding of nothing to the question of the quantum creation of a universe using a Hawking-Turok instanton, which we embedded within the Coleman-De Luccia formalism. We argued that, since up-tunneling from anti-de Sitter space is forbidden, it is impossible to start with nothing and create a universe.…”

Section: Discussionmentioning

confidence: 99%

“…By examining solutions close to the bubble of nothing, we will gain insight into the nature of nothing. Let's begin by studying this approach to the bubble of nothing in the simplest possible model with perturbatively stabilized extra dimensions, the 6D Einstein-Maxwell theory [8,9], a model whose tunneling instantons we constructed explicitly in [10].…”

Section: Bubbles Of Nothing In Stabilized Extra Dimensions: a Simple mentioning

confidence: 99%

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On “nothing” as an infinitely negatively curved spacetime

Brown

Dahlen

2012

Phys. Rev. D

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Nothing-the absence of spacetime-can be either an endpoint of tunneling, as in the bubble of nothing, or a starting point for tunneling, as in the quantum creation of a universe. We argue that these two tunnelings can be treated within a unified framework, and that, in both cases, nothing should be thought of as the limit of anti-de Sitter space in which the curvature length approaches zero. To study nothing, we study decays in models with perturbatively stabilized extra dimensions, which admit not just bubbles of nothing-topology-changing transitions in which the extra dimensions pinch off and a hole forms in spacetime-but also a whole family of topology-preserving transitions that nonetheless smoothly hollow out and approach the bubble of nothing in one limit. The bubble solutions that are close to this limit, bubbles of next-tonothing, give us a controlled setting in which to understand nothing. Armed with this understanding, we are able to embed proposed mechanisms for the reverse process, tunneling from nothing to something, within the relatively secure foundation of the Coleman-De Luccia formalism and show that the Hawking-Turok instanton does not mediate the quantum creation of a universe.

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Section: Discussionmentioning

confidence: 99%

Section: Bubbles Of Nothing In Stabilized Extra Dimensions: a Simple mentioning

confidence: 99%

On “nothing” as an infinitely negatively curved spacetime

Brown

Dahlen

2012

Phys. Rev. D

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“…In the context of a scalar field, such a cascade of classical transitions seems to rely on the existence of roughly evenly spaced vacua in the potential landscape. Interestingly, in [33] it is shown that in a model with multiple vacua constructed from extra dimensions and fluxes, a classical transition is the most natural result, as shown in Figure 14. In these models, the multiple classical transition structure in Figure 13 should be taken seriously.…”

Section: E Multiple Collisionsmentioning

confidence: 98%

How to run through walls: Dynamics of bubble and soliton collisions

et al. 2010

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It has recently been shown in high resolution numerical simulations that relativistic collisions of bubbles in the context of a multi-vacua potential may lead to the creation of bubbles in a new vacuum. In this paper, we show that scalar fields with only potential interactions behave like free fields during high-speed collisions; the kick received by them in a collision can be deduced simply by a linear superposition of the bubble wall profiles. This process is equivalent to the scattering of solitons in 1 + 1 dimensions. We deduce an expression for the field excursion (shortly after a collision), which is related simply to the field difference between the parent and bubble vacua, i.e. contrary to expectations, the excursion cannot be made arbitrarily large by raising the collision energy. There is however a minimum energy threshold for this excursion to be realized. We verify these predictions using a number of 3 + 1 and 1 + 1 numerical simulations. A rich phenomenology follows from these collision induced excursions -they provide a new mechanism for scanning the landscape, they might end/begin inflation, and they might constitute our very own big bang, leaving behind a potentially observable anisotropy.

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“…In this article, we study a simple model (Halliwell [5] and Blanco-Pillado, Schwartz-Perlov, and Vilenkin [6]), which we will call the HBSV model. Let us begin with the six-dimensional action:…”

Section: Flux Compactification In String Theorymentioning

confidence: 99%

The no-boundary measure in string theory: applications to moduli stabilization, flux compactification and cosmic landscape

Hwang

Lee

Sahlmann

et al. 2012

Class. Quantum Grav.

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We investigate the no-boundary measure in the context of moduli stabilization. To this end, we first show that for exponential potentials, there are no classical histories once the slope exceeds a critical value. We also investigate the probability distributions given by the no-boundary wave function near maxima of the potential. These results are then applied to a simple model that compactifies 6D to 4D (HBSV model) with fluxes. We find that the no-boundary wave function effectively stabilizes the moduli of the model. Moreover, we find the a priori probability for the cosmological constant in this model. We find that a negative value is preferred, and a vanishing cosmological constant is not distinguished by the probability measure.We also discuss the application to the cosmic landscape. Our preliminary arguments indicate that the probability of obtaining anti de Sitter space is vastly greater than for de Sitter.

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Quantum tunneling in flux compactifications

Cited by 67 publications

References 48 publications

On “nothing” as an infinitely negatively curved spacetime

On “nothing” as an infinitely negatively curved spacetime

How to run through walls: Dynamics of bubble and soliton collisions

The no-boundary measure in string theory: applications to moduli stabilization, flux compactification and cosmic landscape

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