Publication

A naturally light dilaton

Riccardo Rattazzi, Duccio Pappadopulo, Lorenzo Vitale, Paolo Lodone
2013
Journal Articles

Abstract

Goldstone's theorem does not apply straightforwardly to the case of spontaneously broken scale invariance. We elucidate under what conditions a light scalar degree of freedom, identifiable with the dilaton, can naturally arise. Our construction can be considered an explicit dynamical solution to the cosmological constant problem in the scalar version of gravity.

Official source

https://infoscience.epfl.ch/entities/publication/b5feb600-7952-49e2-87c6-c34982e03c04

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Riccardo Rattazzi, Duccio Pappadopulo, Lorenzo Vitale, Paolo Lodone
2013
Journal Articles

Abstract

Official source

https://infoscience.epfl.ch/entities/publication/b5feb600-7952-49e2-87c6-c34982e03c04

About this result

Related concepts (22)

Cosmological constant

In cosmology, the cosmological constant (usually denoted by the Greek capital letter lambda: Λ), alternatively called Einstein's cosmological constant, is the constant coefficient of a term that Albert Einstein temporarily added to his field equations of general relativity. He later removed it. Much later it was revived and reinterpreted as the energy density of space, or vacuum energy, that arises in quantum mechanics. It is closely associated with the concept of dark energy.

Cosmological constant problem

In cosmology, the cosmological constant problem or vacuum catastrophe is the disagreement between the observed values of vacuum energy density (the small value of the cosmological constant) and theoretical large value of zero-point energy suggested by quantum field theory. Depending on the Planck energy cutoff and other factors, the quantum vacuum energy contribution to the effective cosmological constant is calculated to be between 50 and as much as 120 orders of magnitude greater than observed, a state of affairs described by physicists as "the largest discrepancy between theory and experiment in all of science" and "the worst theoretical prediction in the history of physics".

Flatness problem

The flatness problem (also known as the oldness problem) is a cosmological fine-tuning problem within the Big Bang model of the universe. Such problems arise from the observation that some of the initial conditions of the universe appear to be fine-tuned to very 'special' values, and that small deviations from these values would have extreme effects on the appearance of the universe at the current time. In the case of the flatness problem, the parameter which appears fine-tuned is the density of matter and energy in the universe.

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A naturally light dilaton

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