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Why the de Sitter vacuum cannot fix the MOND acceleration scale: the required moment is the pole of the Riemann zeta function

Preprint. This deposit exists to timestamp a NO-GO result and to carry its reproducibility scripts; it is not a journal publication. It does NOT derive the MOND coefficient and is not a partial derivation -- it closes routes. The result in one line. In a modified-inertia worldlin...

A local, generally covariant field theory of modified inertia

VERSION 3: the static nonlinearity of the delta sector -- v2's sharpest named gap -- is CLOSED, and it closes by a PARITY THEOREM. K IS ODD IN π TO ALL ORDERS. For a static khronon T = t + π(x) the unit normal is nμ = (1/w, −∂iπ/w) with w = √(1−(∂π)2). Under π → −π the normalisat...

A local, generally covariant field theory of modified inertia

VERSION 2: the strong-coupling scale -- v1's sharpest named risk -- is COMPUTED, and it does NOT threaten the phenomenology. Restoring the khronon fluctuation T = t + π gives ln N = −πdot + πdot2/2 + (∂π)2/2, so ai = −∂iπdot and Kij = −∂i∂jπ. At λ = ξ = 1, η = 0 the khronon actio...

Linear Response of the de Sitter Vacuum to Accelerated Matter: A Kubo-Formalism Proof that MOND Requires Non-Equilibrium Physics

Recent attempts to derive Modified Newtonian Dynamics (MOND) and its characteristic acceleration scale a0 rely on the interaction between accelerated matter and the cosmological horizon. A persistent conjecture is that the vacuum response in de Sitter spacetime modifies inertia a...

Linear Response of the de Sitter Vacuum to Accelerated Matter: A Kubo-Formalism Proof that MOND Requires Non-Equilibrium Physics

Recent attempts to derive Modified Newtonian Dynamics (MOND) and its characteristic acceleration scale a0 rely on the interaction between accelerated matter and the cosmological horizon. A persistent conjecture is that the vacuum response in de Sitter spacetime modifies inertia a...

Two Barriers to the MOND Acceleration Coefficient: the de Sitter-Unruh Balance Is Orbital-Invariant at a0 = 2 c H_Lambda, and Rotation-Curve Determinations of a0 Are Definition-Limited at 30%

The MOND acceleration scale a0 is numerically close to c H_Lambda, and several authors have proposed that it is set by the cosmological constant. The relation's form is established (Milgrom 1994, 1999, 2020); its dimensionless O(1) coefficient is not derived by any published argu...

Two Barriers to the MOND Acceleration Coefficient: the de Sitter-Unruh Balance Is Orbital-Invariant at a0 = 2 c H_Lambda, and Rotation-Curve Determinations of a0 Are Definition-Limited at 30%

The MOND acceleration scale a0 is numerically close to c H_Lambda, and several authors have proposed that it is set by the cosmological constant. The relation's form is established (Milgrom 1994, 1999, 2020); its dimensionless O(1) coefficient is not derived by any published argu...

What Can and Cannot Fix the MOND Acceleration Coefficient: a Relabelling Theorem, Three Failed Derivations, and a Redshift Discriminant

The MOND acceleration scale is numerically close to c H_Lambda, and the proposal that it is SET by the cosmological constant dates to Milgrom (1994, 1999). The relation's FORM is established; its dimensionless O(1) COEFFICIENT is not derived by any published argument, and the liv...

The MOND Acceleration Scale as a de Sitter Curvature Scale: Gauged SO(4,1) Gravity Reduces a0 = c^2 sqrt(Lambda/32pi) to a Single Free Number

Galaxy dynamics organize around an acceleration scale a0 ~ 1e-10 m/s^2 that numerically coincides with c*sqrt(Lambda) and cH0. This paper develops the hypothesis that the coincidence is structural -- that a0 is a de Sitter curvature scale, a0 = c^2*sqrt(Lambda/32pi) = (c/2)*sqrt(...