Dynamics of bubbles in general relativity

Berezin, V. A.; Kuzmin, V.; Tkachev, I.

doi:10.1103/physrevd.36.2919

Cited by 284 publications

(349 citation statements)

References 39 publications

Supporting

Mentioning

336

Contrasting

Unclassified

Order By: Relevance

“…10 In vacuum decay problems, 10 This homogeneity property of the AdS background implies that the leading decay process is still given by vacuum CdL bubbles even in the presence of a black hole, since vacuum bubbles nucleated far from the black hole are approximately described by the zero-temperature effective m * is usually governed by the gap of the metastable state, i.e. m * ∼ 1/R + = 1.…”

Section: Measurementioning

confidence: 99%

Holography of AdS vacuum bubbles

Barbón

Rabinovici

2010

J. High Energ. Phys.

View full text Add to dashboard Cite

We consider the fate of AdS vacua connected by tunneling events. A precise holographic dual of thin-walled Coleman-de Luccia bounces is proposed in terms of Fubini instantons in an unstable CFT. This proposal is backed by several qualitative and quantitative checks, including the precise calculation of the instanton action appearing in evaluating the decay rate. Big crunches manifest themselves as time dependent processes which reach the boundary of field space in a finite time. The infinite energy difference involved is identified on the boundary and highlights the ill-defined nature of the bulk setup. We propose a qualitative scenario in which the crunch is resolved by stabilizing the CFT, so that all attempts at crunching always end up shielded from the boundary by the formation of black hole horizons. In all these well defined bulk processes the configurations have the same asymptotics and are finite energy excitations.

show abstract

Section: Measurementioning

confidence: 99%

Holography of AdS vacuum bubbles

Barbón

Rabinovici

2010

J. High Energ. Phys.

View full text Add to dashboard Cite

show abstract

“…In conventional General Relativity, these domain walls separate bubbles of lower vacuum energy from the parent vacuum with higher energy density, and are widely used for cosmological applications (see, e.g. [33]). In modified gravity models with multiple branches, a new possibility arises, where bubbles may catalyze transitions between branches.…”

Section: Hirsute Bubbles: Branch Changelingsmentioning

confidence: 99%

Galileon hairs of Dyson spheres, Vainshtein’s coiffure and hirsute bubbles

Kaloper

Padilla

Tanahashi

2011

J. High Energ. Phys.

View full text Add to dashboard Cite

We study the fields of spherically symmetric thin shell sources, a.k.a. Dyson spheres, in a fully nonlinear covariant theory of gravity with the simplest galileon field. We integrate exactly all the field equations once, reducing them to first order nonlinear equations. For the simplest galileon, static solutions come on six distinct branches. On one, a Dyson sphere surrounds itself with a galileon hair, which far away looks like a hair of any Brans-Dicke field. The hair changes below the Vainshtein scale, where the extra galileon terms dominate the minimal gradients of the field. Their hair looks more like a fuzz, because the galileon terms are suppressed by the derivative of the volume determinant. It shuts off the 'hair bunching' over the 'angular' 2-sphere. Hence the fuzz remains dilute even close to the source. This is really why the Vainshtein's suppression of the modifications of gravity works close to the source. On the other five branches, the static solutions are all singular far from the source, and shuttered off from asymptotic infinity. One of them, however, is really the self-accelerating branch, and the singularity is removed by turning on time dependence. We give examples of regulated solutions, where the Dyson sphere explodes outward, and its self-accelerating side is nonsingular. These constructions may open channels for nonperturbative transitions between branches, which need to be addressed further to determine phenomenological viability of multi-branch gravities.

show abstract

“…Using ordinary formulas of the thin-shell mechanism [7,8] the equation of motion of the shell-Universe has the form:…”

Section: Equation Of Motionmentioning

confidence: 99%

“…Let us use the thin-wall formalism [7,8] and consider a model of shell-Universe expanding in a 5-dimensional spacetime with outer and inner spaces [9] …”

Section: Equation Of Motionmentioning

confidence: 99%