A coupling α is identified with de Sitter entropy via holography and RG flow; imposing monotonic infrared increase on α(k) yields the observed cosmological constant value.
The Cosmological Constant and Lorentz Invariance of the Vacuum State
2 Pith papers cite this work, alongside 15 external citations. Polarity classification is still indexing.
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abstract
One hope to solve the cosmological constant problem is to identify a symmetry principle, based on which the cosmological constant can be reduced either to zero, or to a tiny value. Here, we note that requiring that the vacuum state is Lorentz invariant significantly reduces the theoretical value of the vacuum energy density. Hence, this also reduces the discrepancy between the observed value of the cosmological constant and its theoretical expectation, down from 123 orders of magnitude to 56 orders of magnitude. We find that, at one loop level, massless particles do not yield any contribution to the cosmological constant. Another important consequence of Lorentz symmetry is stabilization of the gravitational hierarchy: the cosmological constant (divided by Newton's constant) does not run as the quartic power of the renormalization group scale, but instead only logarithmically.
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QFT in FLRW spacetime yields a running vacuum energy density ρ_vac(H) that unifies mild dynamical dark energy today with H^4 inflation without an inflaton field.
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Microscopic entropy of de Sitter spacetime and entropic solution to the old cosmological constant problem
A coupling α is identified with de Sitter entropy via holography and RG flow; imposing monotonic infrared increase on α(k) yields the observed cosmological constant value.
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Running Vacuum in the expanding Universe: a unified QFT paradigm for Inflation and Dark Energy
QFT in FLRW spacetime yields a running vacuum energy density ρ_vac(H) that unifies mild dynamical dark energy today with H^4 inflation without an inflaton field.