Flavour Condensates in Brane Models and Dark Energy

TL;DR

This paper explores how string-inspired foam models with D-particles induce flavour mixing and condensates, potentially affecting cosmic acceleration, by analyzing fermionic vacuum expectation values in a curved space-time framework.

Contribution

It evaluates the fermionic flavour vacuum condensate in a string-inspired foam model, linking microscopic interactions to cosmological implications.

Findings

Fermionic vacuum condensate acts as a fluid with negative pressure.

Bosonic contributions are necessary for cosmic acceleration.

D-particle interactions induce non-trivial space-time backgrounds.

Abstract

In the context of a microscopic model of string-inspired foam, in which foamy structures are provided by brany point-like defects (D-particles) in space-time, we discuss flavour mixing as a result of flavour non-preserving interactions of (low-energy) fermionic stringy matter excitations with the defects. Such interactions involve splitting and capture of the matter string state by the defect, and subsequent re-emission. Quantum fluctuations of the D-particles induce a non-trivial space-time background; in some circumstances this could be akin to a cosmological Friedman-Robertson Walker expanding-Universe, with weak (but non-zero) particle production. Furthermore the D-particle medium can induce an MSW type effect. We have argued previously, in the context of bosons, that the so-called flavour vacuum is the appropriate state to be used, at least for low-energy excitations, with energies/momenta up to a dynamically determined cutoff scale. In this work we evaluate the flavour-vacuum expectation value (condensate) of the stress-energy tensor of the (1/2)-spin fields with mixing in an effective low-energy Quantum Field Theory in this foam-induced curved space-time. We demonstrate, at late epochs of the Universe, that the fermionic vacuum condensate behaves as a fluid with negative pressure and positive energy, but alone it cannot lead to present-day accelerating Universes. One needs flavoured boson contributions for this purpose.