Abstract
We consider a finite-size spherical bubble with a nonequilibrium value of the q-field, where the bubble is immersed in an infinite vacuum with the constant equilibrium value q 0 for the q-field (this q 0 has already cancelled an initial cosmological constant). Numerical results are presented for the time evolution of such a q-bubble with gravity turned off and with gravity turned on. For small enough bubbles and a q-field energy scale sufficiently below the gravitational energy scale E Planck , the vacuum energy of the q-bubble is found to disperse completely. For large enough bubbles and a finite value of E Planck , the vacuum energy of the q-bubble disperses only partially and there occurs gravitational collapse near the bubble center.
Highlights
The energy density of the vacuum, the dark energy, and the cosmological constant are highly debated topics today, as quantum field theory suggests a typical number that is some 120 orders of magnitude larger [1,2] than what has been observed [3]
A similar vacuum energy problem exists in condensed-matter systems, and its solution may provide a hint for the solution of the cosmological constant problem
We postpone this analysis to a future publication, as the focus of the present article is on the dispersion of vacuum energy if the Big Bang occurs in a finite region of space surrounded by equilibrium vacuum
Summary
The energy density of the vacuum, the dark energy, and the cosmological constant are highly debated topics today, as quantum field theory suggests a typical number that is some 120 orders of magnitude larger [1,2] than what has been observed [3]. In order to apply this condensed-matter scenario of the cancellation of the vacuum energy to the quantum vacuum of our Universe, we need to know the proper variables to describe this quantum vacuum. One example of such a variable is the four-form field strength used by Hawking in particular [4]. Its value is determined by infrared physics and is proportional either to the matter content of the Universe or to the Hubble expansion rate
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