Dynamics of false-vacuum bubbles

Blau, Steven K.; Guendelman, Eduardo; Guth, Alan H.

doi:10.1103/physrevd.35.1747

Cited by 384 publications

(523 citation statements)

References 39 publications

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“…Typically, these describe spherically symmetric bubbles of "true" vacuum expanding in the "false" vacuum. Occasionally, the reverse is possible, with bubbles of false vacuum forming inside the true vacuum with a small but non-zero probability [30]. In the thin wall limit, which we will consider here, the two vacua are separated by a domain wall, composed of ordinary matter.…”

Section: Jhep12(2008)038mentioning

confidence: 99%

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The instability of vacua in Gauss-Bonnet gravity

Charmousis

Padilla

2008

J. High Energy Phys.

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Owing to the quadratic nature of the theory, Einstein-Gauss-Bonnet gravity generically permits two distinct vacuum solutions. One solution (the "Einstein" vacuum) has a well defined limit as the Gauss-Bonnet coupling goes to zero, whereas the other solution (the "stringy" vacuum) does not. There has been some debate regarding the stability of these vacua, most recently from Deser & Tekin who have argued that the corresponding black hole solutions have positive mass and as such both vacua are stable. Whilst the statement about the mass is correct, we argue that the stringy vacuum is still perturbatively unstable. Simply put, the stringy vacuum suffers from a ghost-like instability that is not excited by the spherically symmetric black hole, but would be excited by any source likely to emit gravitational waves, such as a binary system. This result is reliable except in the strongly coupled regime close to the Chern-Simons limit, when the two vacua are almost degenerate. In this regime, we study instanton transitions between branches via bubble nucleation, and calculate the nucleation probability. This demonstrates that there is large mixing between the vacua, so that neither of them can accurately describe the true quantum vacuum. We also present a new gravitational instanton describing black hole pair production in de Sitter space on the Einstein branch, which is preferred to the usual Nariai instantons and is not present in pure Einstein gravity.

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Section: Jhep12(2008)038mentioning

confidence: 99%

“…If both vacua are de Sitter, we see from case (iv) that tunnelling can occur in the opposite direction, from true to false, but with a very low nucleation rate (see, for example [30]). …”

Section: Jhep12(2008)038mentioning

confidence: 99%

The instability of vacua in Gauss-Bonnet gravity

Charmousis

Padilla

2008

J. High Energy Phys.

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“…(68) appears to contain an ambiguity, since K µν must be evaluated at r = 0 where it is discontinuous. Thus we define the following quantities [9] δK = lim…”

Section: Effective Theory a Linear Regimementioning

confidence: 99%

A quasi-thick codimension 2 braneworld

Kanno

Soda

2004

J. Cosmol. Astropart. Phys.

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We study a codimension 2 braneworld in the Einstein Gauss-Bonnet gravity. We carefully examine the structure of possible singularities in the system which characterize the braneworld through matching conditions. Consequently, we find that the thickness of the brane can be incorporated as the distributional source, which we dub quasi-thickness. On the basis of our formalism, we analyze the linearized gravity and show the conventional Einstein gravity can be recovered on the brane. In the nonlinear regime, however, we find corrections due to the thickness and the bulk geometry. We also point out a possibility that the thickness plays a role of the dark energy/dark matter in the universe.

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“…Kraus and Wilczek employ the system of coordinates τ and r in the external Kruskal spacetime (M 2 , E + ) that has been defined in Sec. 3 (formula (8)). The relations (60) and (8) imply that the retarded time u + can be expressed by means of τ as follows:…”

Section: Out-side Storymentioning

confidence: 99%

Gauge-invariant Hamiltonian formalism for spherically symmetric gravitating shells

Hájı́ček

Bičák

1997

Phys. Rev. D

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The dynamics of a spherically symmetric thin shell with arbitrary rest mass and surface tension interacting with a central black hole is studied. A careful investigation of all classical solutions reveals that the value of the radius of the shell and of the radial velocity as an initial datum does not determine the motion of the shell; another configuration space must, therefore, be found. A different problem is that the shell Hamiltonians used in literature are complicated functions of momenta (non-local) and they are gauge dependent. To solve these problems, the existence is proved of a gauge invariant super-Hamiltonian that is quadratic in momenta and that generates the shell equations of motion. The true Hamiltonians are shown to follow from the super-Hamiltonian by a reduction procedure including a choice of gauge and solution of constraint; one important step in the proof is a lemma stating that the true Hamiltonians are uniquely determined (up to a canonical transformation) by the equations of motion of the shell, the value of the total energy of the system, and the choice of time coordinate along the shell. As an example, the Kraus-Wilczek Hamiltonian is rederived from the super-Hamiltonian. The super-Hamiltonian coincides with that of a fictitious particle moving in a fixed two-dimensional Kruskal spacetime under the influence of two effective potentials. The pair consisting of a point of this spacetime and a unit timelike vector at the point, considered as an initial datum, determines a unique motion of the shell.

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Dynamics of false-vacuum bubbles

Cited by 384 publications

References 39 publications

The instability of vacua in Gauss-Bonnet gravity

The instability of vacua in Gauss-Bonnet gravity

A quasi-thick codimension 2 braneworld

Gauge-invariant Hamiltonian formalism for spherically symmetric gravitating shells

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