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Effective Field Theory, Black Holes, and the Cosmological Constant
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Bekenstein has proposed the bound S < pi M_P^2 L^2 on the total entropy S in a volume L^3. This non-extensive scaling suggests that quantum field theory breaks down in large volume. To reconcile this breakdown with the success of local quantum field theory in describing observed particle phenomenology, we propose a relationship between UV and IR cutoffs such that an effective field theory should be a good description of Nature. We discuss implications for the cosmological constant problem. We find a limitation on the accuracy which can be achieved by conventional effective field theory: for example, the minimal correction to (g-2) for the electron from the constrained IR and UV cutoffs is larger than the contribution from the top quark.
Forward citations
Cited by 23 Pith papers
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Matrix Multiverses Meet Multiple Mythologies
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Quantum Geometry from Area Fluctuations
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Geometric noise spectrum in interferometers
The noise spectrum an interferometer would see from quantum spacetime jitter is computed for vacuum, thermal, squeezed, and scalar-backreaction states; all are Planck-suppressed.
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Diamonds in the Bulk and Large-$N$ Scaling in AdS/CFT
Bulk field algebras of causal diamonds in AdS/CFT require a double-scaling limit, so sub-AdS-radius distances are not described by bulk QFT.
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Holographic bounce
Holographic infrared and ultraviolet cutoffs can produce bouncing solutions, including nonsingular ones, and can be designed to reproduce F(R) gravity bounce.
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Why There is No Memory Burden in Holographic Space-time Models of Black Hole Formation and Evaporation
In the author's holographic space-time toy model, black hole evaporation is not slowed by memory burden because decay phase space overcomes the entropy cost of frozen q-bits.
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Phantom-Divide Crossing in Barrow-Tsallis Holographic Dark Energy with a Scale-Dependent Barrow Exponent
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Measuring neutrino mass in light of ACT DR6 and DESI DR2
New ACT and DESI data yield model-dependent upper limits on sum of neutrino masses, with holographic dark energy giving the tightest bounds and a consistent preference for degenerate hierarchy.
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Light scalars in light of UV/IR mixing: classicalization via synergy between Vainshtein and chameleon screenings
Classicalizing k-essence scalars need m << Λ* and, when potentials or fermion couplings are present, a chameleon-like screening layer to keep Vainshtein screening and classicalon stability intact.
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Constraints on Barrow and Tsallis Holographic Dark Energy from DESI DR2 BAO data
Barrow and Tsallis holographic dark energy models fit DESI DR2 data but are disfavored by information criteria versus LambdaCDM and do not ease the Hubble tension.
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The Hydrodynamic Approach to Quantum Gravity
Banks proposes and summarizes a holographic space-time framework in which Einstein's equations emerge as hydrodynamics of quantum systems associated to causal diamonds, with a conjectured quantum principle of relativity.
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Late-time cosmological constraints on three holographic dark energy models with DESI DR2 BAO and Type Ia supernovae
DESI DR2 and late-time data constrain HDE, ADE and RDE, yielding H0≈67–68 km/s/Mpc, c≈1, n≈2.8, γ≈0.54, with none resolving the Hubble tension or decisively beating ΛCDM.
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Candidate collapse-noise correlators from Generalized Trace Dynamics: a Hubble-scale spectral line under structural assumptions
Under explicit auxiliary structural postulates, Generalized Trace Dynamics yields a candidate CSL-type collapse-noise two-point function with a narrow Wightman line at twice the Hubble scale.
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What does it mean to have a quantum gravitational theory of de Sitter Space?
De Sitter space modeled as a finite quantum system yields ambiguous theories, with local experiments accessing only a tiny fraction of its total information content.
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Field theory vacuum and entropic dark energy models
The paper derives new dark energy models from the postulate that the arbitrary oscillator mass in a free field's Hamiltonian is a real, gravitating mass contributing vacuum energy density μK^3.
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Barrow holographic dark energy interacting model in the presence of radiation and matter
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Addendum: Fitting the DESI BAO Data with Dark Energy Driven by the Cohen-Kaplan-Nelson Bound
Updating to DESI DR2, the CKN-motivated dark-energy models fit better than Lambda-CDM by up to about 2.6 sigma, while omega-CDM-type models fit even better.
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Hilbert Bundles and Holographic Space-time: the Hydrodynamic Approach to Gravity
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The Awada-Gibbons-Shaw Algebra in de Sitter Space and SUSY Breaking
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A short overview on the Black Hole-Tower Correspondence and Species Thermodynamics
A review of the black hole-tower correspondence and species thermodynamics, which aim to explain black hole entropy via towers of light states and to show only certain towers are allowed.
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Exploring Hubble Tension Alleviation through Neutrino-Coupled Perturbed $f(R)$ Gravity
A fit of Hu-Sawicki f(R) gravity with a fitted neutrino interaction to CMB, lensing, BAO, CC, and Pantheon data returns H0 near 70 km/s/Mpc, partially easing but not resolving the Hubble and S8 tensions.
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