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AQUAL

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AQUAL is a theory of gravity based on Modified Newtonian Dynamics (MOND), but using a Lagrangian. It was developed by Jacob Bekenstein and Mordehai Milgrom in their 1984 paper, "Does the missing mass problem signal the breakdown of Newtonian gravity?",^[1] as well as a 1986 paper by Milgrom.^[2] "AQUAL" stands for "AQUAdratic Lagrangian", stemming from the fact that, in contrast to Newtonian gravity, the proposed Lagrangian is non-quadratic in the potential gradient $|\nabla \Phi |$ .

The gravitational force law obtained from MOND,

m\mu \left({\frac {a}{a_{0}}}\right)a={\frac {GMm}{r^{2}}},

has a serious defect: it violates Newton's third law of motion, and therefore fails to conserve momentum and energy.^[3] To see this, consider two objects with $m\neq M$ ; then we have:

\mu \left({\frac {a_{m}}{a_{0}}}\right)ma_{m}={\frac {GMm}{r^{2}}}={\frac {GMm}{r^{2}}}=\mu \left({\frac {a_{M}}{a_{0}}}\right)Ma_{M}

but the third law gives $ma_{m}=Ma_{M},$ so we would get

\mu \left({\frac {a_{m}}{a_{0}}}\right)=\mu \left({\frac {a_{M}}{a_{0}}}\right)

even though $a_{m}\neq a_{M},$ and $\mu$ would therefore be constant, contrary to the MOND assumption that it is non-linear for small arguments.

This problem can be rectified by deriving the force law from a Lagrangian, at the cost of possibly modifying the general form of the force law. Then conservation laws could then be derived from the Lagrangian by the usual means.

The AQUAL Lagrangian is:

\rho \Phi +{\frac {1}{8\pi G}}a_{0}^{2}F\left({\frac {|\nabla \Phi |^{2}}{a_{0}^{2}}}\right);

this leads to a modified Poisson equation:

\nabla \cdot \left(\mu \left({\frac {|\nabla \Phi |}{a_{0}}}\right)\nabla \Phi \right)=4\pi G\rho ,\qquad {\text{with }}\quad \mu (x)={\frac {dF(x^{2})}{dx}}.

where the predicted acceleration is $-\nabla \Phi =a.$ These equations reduce to the MOND equations in the spherically symmetric case, although they differ somewhat in the disc case needed for modelling spiral or lenticular galaxies. However, the difference is only 10–15%, so does not seriously impact the results.

According to Sanders and McGaugh, one problem with AQUAL (or any scalar–tensor theory in which the scalar field enters as a conformal factor multiplying Einstein's metric) is AQUAL's failure to predict the amount of gravitational lensing actually observed in rich clusters of galaxies.^[4] AQUAL has been claimed to match observations of wide binary star orbits.^[5]

References

[edit]

^ Jacob Bekenstein & M. Milgrom (1984). "Does the missing mass problem signal the breakdown of Newtonian gravity?". Astrophys. J. 286: 7–14. Bibcode:1984ApJ...286....7B. doi:10.1086/162570.
^ Milgrom, M (1986). "Solutions for the modified Newtonian dynamics field equation". Astrophys. J. 302: 617–625. Bibcode:1986ApJ...302..617M. doi:10.1086/164021.
^ Felten, J. E. (1984). "Milgrom's revision of Newton's laws - Dynamical and cosmological consequences". The Astrophysical Journal. 286: 3. doi:10.1086/162569. ISSN 0004-637X.
^ Sanders, Robert H.; McGaugh, Stacy S. (2002). "Modified Newtonian dynamics as an alternative to dark matter". Annual Review of Astronomy and Astrophysics. 40 (1): 263–317. arXiv:astro-ph/0204521. Bibcode:2002ARA&A..40..263S. doi:10.1146/annurev.astro.40.060401.093923.
^ Chae, Kyu-Hyun (2023-08-01). "Breakdown of the Newton–Einstein Standard Gravity at Low Acceleration in Internal Dynamics of Wide Binary Stars". The Astrophysical Journal. 952 (2): 128. arXiv:2305.04613. doi:10.3847/1538-4357/ace101. ISSN 0004-637X.

Theories of gravitation

Standard

Newtonian gravity (NG)	Newton's law of universal gravitation Gauss's law for gravity Poisson's equation for gravity History of gravitational theory
General relativity (GR)	Introduction History Mathematics Exact solutions Resources Tests Post-Newtonian formalism Linearized gravity ADM formalism Gibbons–Hawking–York boundary term

Alternatives to
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Paradigms	Classical theories of gravitation Quantum gravity Theory of everything
Classical	Poincaré gauge theory Einstein–Cartan Teleparallelism Bimetric theories Gauge theory gravity Composite gravity f(R) gravity Infinite derivative gravity Massive gravity Modified Newtonian dynamics, MOND AQUAL Tensor–vector–scalar Nonsymmetric gravitation Scalar–tensor theories Brans–Dicke Scalar–tensor–vector Conformal gravity Scalar theories Nordström Whitehead Geometrodynamics Induced gravity Degenerate Higher-Order Scalar-Tensor theories
Quantum-mechanical	Euclidean quantum gravity Canonical quantum gravity Wheeler–DeWitt equation Loop quantum gravity Spin foam Causal dynamical triangulation Asymptotic safety in quantum gravity Causal sets DGP model Rainbow gravity theory
Unified-field-theoric	Kaluza–Klein theory Supergravity
Unified-field-theoric and quantum-mechanical	Noncommutative geometry Semiclassical gravity Superfluid vacuum theory Logarithmic BEC vacuum String theory M-theory F-theory Heterotic string theory Type I string theory Type 0 string theory Bosonic string theory Type II string theory Little string theory Twistor theory Twistor string theory
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from Grokipedia

AQUAL, short for AQuadratic Lagrangian, is a nonrelativistic field theory formulation of Modified Newtonian Dynamics (MOND) that modifies the standard Newtonian description of gravity to explain observed discrepancies in galactic dynamics, such as flat rotation curves, without invoking dark matter.^[1] Developed by Jacob Bekenstein and Mordehai Milgrom in 1984, it achieves this by altering the gravitational Lagrangian from the conventional quadratic form in the gradient of the potential to a more general nonlinear function, allowing a smooth interpolation between Newtonian gravity at high accelerations and MOND behavior at low accelerations below a critical scale

a_0 \approx 1.2 \times 10^{-10}

m/s².^[1]^[2] The core of AQUAL lies in its action principle, expressed through the Lagrangian density

\mathcal{L} = \rho \phi - F(|\nabla \phi|^2 / a_0^2)

, where

\rho

is the matter density,

\phi

is the gravitational potential,

a_0

sets the MOND acceleration scale, and

F

is an interpolating function chosen such that

F(x) \approx x

for

x \gg 1

(recovering Newtonian gravity) and

F(x) \approx \sqrt{x}

F(x)≈x

for $x \ll 1$ (yielding the MOND deep-limit force law $\mathbf{g} \cdot \mathbf{g}_N = a_0$ , with $\mathbf{g}_N$ the Newtonian field).^[2] This leads to a nonlinear Poisson equation $\nabla \cdot [\mu(|\nabla \phi|/a_0) \nabla \phi] = 4\pi G \rho$ , where $\mu(y) = y F'(y^2)/2$ acts as an effective interpolating function between linear (Newtonian) and constant (MOND) regimes.^[1] Unlike the original MOND postulate, which directly modifies Newton's second law, AQUAL's Lagrangian approach ensures conservation of momentum and energy in isolated systems, though it introduces complexities in multi-galaxy interactions due to the nonlinearity.^[3] AQUAL has demonstrated success in predicting rotation curves for disk galaxies and the kinematics of dwarf spheroidals using only visible baryonic matter, aligning with observations better than Newtonian models in many cases.^[4] However, it encounters challenges in reproducing the external field effect in wide binaries and globular clusters, as well as in cosmological contexts like structure formation, prompting extensions such as the relativistic Tensor-Vector-Scalar (TeVeS) theory.^[4]^[5] Despite these limitations, AQUAL remains a foundational framework for testing MOND paradigms and exploring alternatives to dark matter on galactic scales.^[2]

Background and History

Modified Newtonian Dynamics (MOND)

Modified Newtonian Dynamics (MOND) emerged as a response to the observed discrepancies in galactic dynamics, particularly the flat rotation curves of spiral galaxies, where orbital velocities remain roughly constant at large radii rather than declining as predicted by Newtonian gravity for visible matter alone. These observations, first systematically documented in the 1970s, implied a mass discrepancy that could not be accounted for by luminous baryonic matter, prompting alternatives to the dark matter hypothesis.^[6] MOND posits that the laws of dynamics themselves require modification in regions of low acceleration, providing a framework to explain these phenomena without invoking unseen mass.^[7] Proposed by Mordehai Milgrom in 1983, MOND's core postulate is that Newton's second law is altered for accelerations below a characteristic scale

a_0

of order

10^{-8}

cm s

^{-2}

(or

10^{-10}

m s

^{-2}

), transitioning from the standard Newtonian regime at high accelerations to a modified regime at low accelerations.^[7] This modification is encapsulated in an interpolating function

\mu(x)

, where

x = |a|/a_0

, such that

\mu(x) \approx x

for

x \ll 1

(deep-MOND limit) and

\mu(x) \approx 1

for

x \gg 1

(Newtonian limit).^[8] The value of

a_0

has been refined through fits to rotation curve data to

\approx 1.2 \times 10^{-10}

m s

^{-2}

, confirming its universality across galaxies.^[8] A key prediction of MOND is the mass-discrepancy-acceleration relation (MDAR), expressed as

g / g_N = \mu(|g_N|/a_0)

, where

g

is the actual acceleration,

g_N

is the Newtonian acceleration due to baryonic matter, and the relation holds without adjustable parameters beyond

a_0

.^[8] This leads to flat rotation curves in the low-acceleration outskirts of galaxies, matching observations more naturally than dark matter models in many cases.^[7] AQUAL provides a Lagrangian-based field theory realization of these MOND principles, ensuring consistency with conservation laws.^[9]

Development of AQUAL

AQUAL, or the A QUAdratic Lagrangian theory, was proposed in 1984 by Jacob Bekenstein and Mordehai Milgrom as a field-theoretic formulation of Modified Newtonian Dynamics (MOND), which had demonstrated empirical success in explaining galaxy rotation curves without dark matter.^[9] The primary motivation was to resolve MOND's limitations in handling multi-body systems and ensuring conservation of momentum, angular momentum, and energy, which were problematic in its original non-relativistic, non-Lagrangian form.^[9] By introducing a nonlinear scalar field theory with a Lagrangian density, AQUAL provided a consistent framework that recovered Newtonian gravity in high-acceleration regimes while modifying dynamics at low accelerations.^[9] The theory was detailed in their seminal paper published in The Astrophysical Journal, where Bekenstein and Milgrom derived the modified field equations from the action principle, emphasizing the non-quadratic kinetic term that distinguished it from standard theories.^[9] This formulation inherently incorporated the external field effect (EFE), whereby an external gravitational field influences internal dynamics, addressing inconsistencies in isolated system assumptions.^[9] Subsequent refinements in the late 1980s and early 1990s by Milgrom and collaborators focused on numerical implementations and consistency checks with multi-galaxy systems, solidifying AQUAL's role as a foundational MOND extension. Early recognition of AQUAL highlighted its innovative departure from quadratic Lagrangians in field theories, earning the "aquadratic" moniker for the interpolation function that nonlinearly couples the gravitational potential to matter density.^[9] This conceptual evolution marked a shift toward Lagrangian-based modifications of gravity, paving the way for relativistic generalizations while maintaining MOND's core empirical motivations.^[9]

Theoretical Formulation

Lagrangian Density

The AQUAL theory is formulated via an action principle, with the total action

S = \int \mathrm{d}t \int \mathrm{d}^3x \left[ -\rho \phi - \frac{a_0^2}{8\pi G} F\left( \frac{|\nabla \phi|^2}{a_0^2} \right) \right],

where

\phi

is the scalar gravitational potential,

\rho

is the baryonic mass density,

G

is Newton's gravitational constant, and

a_0

is the critical acceleration scale (

a_0 \approx 1.2 \times 10^{-10}

m s

^{-2}

).^[1] The scalar potential

\phi

generates the gravitational field

\mathbf{g} = -\nabla \phi

, to which the baryonic density

\rho

couples linearly in the matter Lagrangian term

-\rho \phi

.^[1] The function

F(z)

in the gravitational Lagrangian term is a dimensionless interpolating function of the dimensionless argument

z = |\nabla \phi|^2 / a_0^2

, designed to recover standard Newtonian gravity in the high-acceleration regime while transitioning to modified dynamics at low accelerations. Specifically,

F(z) \approx z

for

z \gg 1

(ensuring the Newtonian limit where the field equations reduce to the standard Poisson equation

\nabla^2 \phi = 4\pi G \rho

) and

F(z) \approx \frac{2}{3} z^{3/2}

for

z \ll 1

(the deep-MOND regime, which enforces scale invariance under

(\mathbf{r}, t, a_0) \to \lambda (\mathbf{r}, t, a_0)

).^[1] The MOND interpolating function

\mu(x)

(with

x = |\nabla \phi| / a_0

) emerges from the gravitational Lagrangian as

\mu(x) = F'(x^2)

, ensuring consistency with the original MOND prescription where

\mu(x) \approx 1

for

x \gg 1

and

\mu(x) \approx x

for

x \ll 1

.^[1] This structure preserves the conservation of momentum and angular momentum while modifying the gravitational field equations nonlinearly.^[1]

Nonlinear Field Equations

The nonlinear field equations of AQUAL are derived by varying the action with respect to the gravitational potential

\phi

, yielding the modified Poisson equation

\nabla \cdot \left[ \mu\left( \frac{|\nabla \phi|}{a_0} \right) \nabla \phi \right] = 4\pi G \rho

, where

\rho

is the mass density,

G

is Newton's constant,

a_0

is the fundamental acceleration scale (

\approx 1.2 \times 10^{-10}

m s

^{-2}

), and

\mu(x) = F'(x^2)

, with

F

the nonlinear function appearing in the Lagrangian density.^[10] In the Newtonian limit, where accelerations are much larger than

a_0

(i.e.,

x \gg 1

\mu(x) \approx 1

, reducing the equation to the standard Poisson equation

\nabla^2 \phi = 4\pi G \rho

and recovering general relativity's weak-field behavior.^[10] In the deep-MOND limit, for accelerations much smaller than

a_0

(i.e.,

x \ll 1

\mu(x) \approx x

, so the equation simplifies to

\nabla \cdot \left( \frac{|\nabla \phi| \nabla \phi}{a_0} \right) = 4\pi G \rho

, or equivalently

\nabla \cdot (|\mathbf{g}| \mathbf{g}) = 4\pi G a_0 \rho

where

\mathbf{g} = -\nabla \phi

, leading to an effective gravitational field strength

g \propto \sqrt{G M a_0}/r

g∝GMa0

/r for a point mass $M$ .^[10] The inherent nonlinearity of these equations, stemming from the dependence of $\mu$ on the gradient of $\phi$ , introduces significant challenges in solving for systems with multiple mass sources, as the field from one source influences the $\mu$ factor and thus the field from others, resulting in nonlocal effects that complicate analytical and numerical treatments.^[10]

Relation to MOND and Key Features

Implementation of MOND Interpolation

In the AQUAL formulation, the interpolation between Newtonian and MOND regimes is achieved through a dimensionless function

\mu(x)

, where

x = |\nabla \phi| / a_0

and

a_0

is the characteristic MOND acceleration scale, approximately

1.2 \times 10^{-10}

m/s². This function modifies the gravitational field equation to ensure that in regions of high acceleration (

x \gg 1

\mu(x) \approx 1

, recovering the standard Poisson equation

\nabla^2 \phi = 4\pi G \rho

and thus Newtonian gravity. Conversely, in the deep-MOND regime of low acceleration (

x \ll 1

\mu(x) \approx x

, leading to an enhanced gravitational response that scales nonlinearly with the source density

\rho

.^[9] The physical acceleration

\mathbf{g} = -\nabla \phi

satisfies the nonlinear field equation

\nabla \cdot [\mu(|\nabla \phi|/a_0) \nabla \phi] = 4\pi G \rho

, which interpolates smoothly between the two limits over accelerations near

a_0

. In spherically symmetric or otherwise simple geometries, this reduces to an algebraic relation

\mu(g/a_0) \mathbf{g} = \mathbf{g}_N

, where

\mathbf{g}_N = -\nabla \phi_N

is the Newtonian acceleration satisfying

\nabla^2 \phi_N = 4\pi G \rho

. This relation ensures that the physical field

\mathbf{g}

is a monotonic deformation of the Newtonian field, preserving the direction of gravity while amplifying its magnitude in weak fields.^[9] In the deep-MOND limit for a point mass

M

, the Newtonian field is

g_N = G M / r^2

, so the relation

\mu(g/a_0) g \approx g_N

with

\mu \approx g/a_0

yields

g^2 / a_0 \approx g_N

, or

g \approx \sqrt{G M a_0}/r

g≈GMa0

/r. This reproduces MOND's modification of Newton's second law, where the effective gravitational force on a test particle yields asymptotically flat rotation curves for galaxies, with orbital speeds $v \approx (G M a_0)^{1/4}$ .^[9] For isolated single-body systems, the algebraic relation $\mu(g/a_0) g = g_N$ directly links the physical and Newtonian fields, ensuring consistent dynamics without additional parameters. Unlike the original phenomenological MOND, which modified Newton's second law non-variationally and struggled with conservation laws and multi-body interactions, AQUAL's Lagrangian origin enforces momentum conservation and naturally incorporates the external field effect (EFE), where an ambient external acceleration suppresses the internal MOND enhancement if it exceeds $a_0$ . This makes AQUAL better suited for systems like galaxies in clusters, where external fields influence dynamics.^[9]

Scale Invariance and External Field Effect

In the deep-MOND limit of AQUAL, where internal accelerations are much less than the fundamental scale

a_0

, the theory exhibits space-time scale invariance.^[11] This symmetry manifests under the transformation

\phi \to \lambda^{-1} \phi

t \to \lambda t

x \to \lambda x

, with

a_0

fixed, for any positive

\lambda

, ensuring that the equations of motion remain unchanged.^[11] As a result, orbital velocities for isolated systems scale as

v \propto (G M a_0)^{1/4}

, independent of the system's size, which underpins the universal form of rotation curves in the low-acceleration regime.^[11] The external field effect (EFE) in AQUAL arises when an external gravitational acceleration

g_\mathrm{ext}

influences a system's internal dynamics, even if the external source is distant.^[12] If the Newtonian internal acceleration

g_N \ll g_\mathrm{ext}

, the interpolation function satisfies

\mu(x) \approx g_\mathrm{ext} / a_0

, effectively suppressing the MOND boost and forcing internal motions to approximate Newtonian behavior scaled by

G_\mathrm{eff} \sim G a_0 / g_\mathrm{ext}

.^[12] This effect is prominent in systems like wide binaries in the Solar neighborhood or dwarf galaxies near hosts, where

g_\mathrm{ext}

from the Milky Way dominates.^[13] Mathematically, the EFE originates from the nonlinearity of AQUAL's field equation, which couples the gradients of the internal potential to those of the external field through the shared interpolation function.^[12] Observationally, the EFE provides explanations for phenomena such as the quasi-Newtonian dynamics observed in low-surface-brightness galaxies embedded in strong external fields from nearby groups, where internal MOND effects are quenched.^[14] It also accounts for velocity dispersions in dwarf spheroidal satellites that align better with EFE-modified predictions than pure deep-MOND expectations.^[15] These features emerge directly from the MOND interpolation mechanism implemented in AQUAL's Lagrangian.^[12]

Predictions and Astrophysical Applications

Galaxy Rotation Curves

In the framework of AQUAL, the modified gravitational dynamics leads to asymptotically flat rotation curves for isolated galaxies at large radii, where the acceleration falls below the characteristic scale

a_0 \approx 1.2 \times 10^{-10}

m s

^{-2}

. Specifically, for a point mass

M

, the circular velocity satisfies

v^2(r) \to \sqrt{G M a_0}

v2(r)→GMa0

in the deep-MOND regime, yielding a constant velocity independent of radius and matching the observed flat profiles in spiral galaxies such as the Milky Way.^[16] This prediction arises from the nonlinear Poisson equation in AQUAL, where the gravitational field strength $g$ scales as $\sqrt{a_0 g_N}$

for $g \ll a_0$ , with $g_N$ the Newtonian field, ensuring the rotation curve transitions smoothly from Keplerian behavior at small radii to flatness outward. Numerical solutions of the AQUAL field equations for axisymmetric mass distributions, such as thin disks representing galactic baryonic matter, demonstrate this transition explicitly. These solutions solve the nonlinear equation $\nabla \cdot (\mu(|\nabla \Phi|/a_0) \nabla \Phi) = 4\pi G \rho$ , where $\mu(x) \approx x$ for $x \ll 1$ , revealing rotation curves that rise steeply near the center before flattening, consistent with observed profiles in spirals without invoking dark matter.^[17] Such computations highlight the theory's ability to reproduce the inner Keplerian regime ( $v \propto r^{-1/2}$ ) and the outer flat regime for realistic density profiles, with the interpolation function $\mu$ ensuring continuity. AQUAL has successfully fitted the rotation curves of approximately 100 galaxies using only their observed baryonic mass distributions, often employing quasi-linear approximations like QUMOND to facilitate computations while approximating the full nonlinear AQUAL results. These fits, applied to samples of spiral and low-surface-brightness galaxies, achieve high accuracy across a range of luminosities and morphologies, outperforming Newtonian models without dark matter and rivaling dark matter fits in simplicity. For instance, QUMOND-based modeling of axisymmetric disks yields velocity profiles that align closely with HI observations, with typical residuals below 10% in the flat regime.^[18] In tidally limited systems like dwarf galaxies, the external field effect (EFE) in AQUAL causes rotation curves to deviate from the deep-MOND asymptotic flatness, as the external acceleration from a host galaxy suppresses the internal MOND boost when it exceeds $a_0$ . This results in more Newtonian-like profiles for dwarfs in strong external fields, such as those orbiting the Milky Way, where velocities rise less steeply and may decline outward, explaining observed variations without additional components.^[19] Numerical AQUAL simulations confirm that the EFE strength, derived from the cosmic environment, aligns with these deviations, providing a natural account for the diversity in dwarf rotation curves.^[17]

Baryonic Tully-Fisher Relation

In the deep-MOND limit of AQUAL, applicable to isolated galaxies where internal accelerations are much less than the fundamental scale

a_0 \approx 1.2 \times 10^{-10}

m s

^{-2}

, the theory predicts the baryonic Tully-Fisher relation (BTFR) through its nonlinear field equations. The gravitational field strength

g

satisfies

\mu(g/a_0) g = g_N

, where

g_N = G M_b / r^2

is the Newtonian field from the total baryonic mass

M_b

, and the interpolating function

\mu(x) \approx x

for

x \ll 1

. This yields

g \approx \sqrt{g_N a_0}

g≈gNa0

, and for a flat rotation curve where the circular velocity $V$ satisfies $V^2 / r = g$ , the relation simplifies to $V^4 = G M_b a_0.$ ^[8] This derivation emerges directly from the aquadratic Lagrangian formulation of AQUAL, which modifies the Poisson equation to $\nabla \cdot [ \mu(|\nabla \Phi|/a_0) \nabla \Phi ] = 4\pi G \rho_b$ , ensuring the asymptotic velocity scales as the fourth root of the enclosed baryonic mass in the low-acceleration regime. Unlike Newtonian gravity augmented by dark matter, AQUAL requires no additional mass component, with the BTFR arising as a fundamental consequence of the scale-dependent dynamics.^[8] Observationally, the BTFR holds tightly for spiral and irregular galaxies across more than five decades in baryonic mass, from low-mass dwarfs ( $M_b \sim 10^7 M_\odot$ ) to massive spirals ( $M_b \sim 10^{11} M_\odot$ ), with the predicted slope of 4 confirmed to high precision.^[8] Studies of gas-rich systems, using extended rotation curves and HI mapping, demonstrate that the relation aligns with AQUAL predictions without systematic deviations, yielding an intrinsic scatter consistent with zero within measurement uncertainties—typically $\Delta V / V \lesssim 0.04$ or less than 20% in velocity space.^[20] The nonlinearity inherent to AQUAL's field equations ensures this remarkable tightness by imposing a universal force law that minimizes sensitivity to variations in baryonic mass distributions, such as differences in stellar or gas profiles across galaxy types.^[8] In dark matter models, achieving a similarly precise BTFR requires fine-tuning of halo properties and baryon-dark matter interactions, whereas AQUAL derives it naturally from the modified dynamics alone, without adjustable parameters beyond $a_0$ .^[8]^[20] For low-mass galaxies, the external field effect (EFE) in AQUAL introduces deviations from the isolated BTFR, as the ambient acceleration from the host environment ( $g_\mathrm{ext} \sim 10^{-10}$ m s $^{-2}$ ) can dominate if internal accelerations fall below this threshold.^[8] In such cases, the effective interpolating function shifts toward the quasi-Newtonian regime, reducing maximum velocities and flattening the low-mass end of the relation, consistent with observations of dwarf irregulars in group environments. This EFE modification preserves the overall BTFR integrity while accounting for environmental influences, distinguishing AQUAL's predictions from simpler MOND approximations.^[8]

Relativistic Extensions

Tensor-Vector-Scalar (TeVeS) Theory

Tensor-Vector-Scalar (TeVeS) theory, developed by Jacob Bekenstein in 2004, serves as a primary relativistic generalization of the A Quadratic Lagrangian (AQUAL) framework within the Modified Newtonian Dynamics (MOND) paradigm.^[5] It addresses the need for a covariant theory that recovers MOND phenomenology in weak gravitational fields while maintaining consistency with general relativity in strong-field regimes, such as the solar system. In the non-relativistic limit, TeVeS reduces to AQUAL, ensuring compatibility with established MOND predictions for galactic dynamics.^[5] The theory incorporates three dynamical gravitational fields: a tensor field represented by the metric

g_{\mu\nu}

, a vector field

U^\mu

constrained to be unit timelike with respect to

g_{\mu\nu}

(i.e.,

g_{\alpha\beta} U^\alpha U^\beta = -1

), and a scalar field

\phi

that generalizes the AQUAL scalar potential.^[5] These fields couple through a disformal metric

\tilde{g}_{\alpha\beta} = e^{-2\phi} g_{\alpha\beta} - 2 \sinh(2\phi) U_\alpha U_\beta

, which defines the physical metric experienced by matter.^[5] The action for TeVeS consists of an Einstein-Hilbert term for the tensor field, a scalar action involving the nondynamical scalar

\sigma

and the function

F(\mu)

(with

\mu

related to the scalar gradient), and a vector action proportional to the vector field's twist squared, parameterized by constants

k

K

, and a length scale

\ell

.^[5] This formulation ensures Lorentz invariance with respect to the physical metric

\tilde{g}_{\mu\nu}

, positive energy densities for all fields, and the reproduction of MOND behavior in the weak-field limit where accelerations fall below

a_0 \approx 10^{-8}

cm/s².^[5] Recent work has explored connections between TeVeS and mimetic gravity theories, potentially extending its applicability in relativistic MOND frameworks.^[21]

Conservation Principles in Relativistic MOND

In the AQUAL formulation of Modified Newtonian Dynamics (MOND), momentum conservation is achieved by assigning a portion of the total momentum to the gravitational field itself, rather than solely to the matter particles. This approach addresses the non-conservation issues inherent in the original MOND postulate, where the modified force law could lead to apparent violations of Newton's third law for interacting bodies. Locally, the theory violates the standard form of Newton's third law, as the forces between particles are not equal and opposite due to the nonlinear nature of the field equations; however, global conservation of total momentum (matter plus field) is preserved through the field's contribution. In relativistic extensions such as TeVeS, which recovers AQUAL in the non-relativistic limit, similar mechanisms ensure the conservation of the energy-momentum tensor via contributions from the tensor, vector, and scalar fields. These field contributions maintain diffeomorphism invariance, a key requirement for a consistent relativistic gravity theory, by allowing the action to be generally covariant. However, this structure leads to violations of the strong equivalence principle, as the inertial and gravitational properties of self-gravitating systems become dependent on the external gravitational environment through the scalar field's coupling, distinguishing TeVeS from general relativity.^[22] These conservation features have significant implications for modeling binary systems, where the field's momentum can induce subtle deviations in the center-of-mass motion and orbital evolution compared to Newtonian expectations, requiring careful treatment to avoid artificial momentum drifts. In N-body simulations of MONDian systems, such as star clusters or galaxies, the nonlinear field equations must be solved on a spatial grid (e.g., using particle-mesh methods) to accurately incorporate the field momentum, ensuring global conservation while handling the computational challenges of the theory's nonlinearity.

Criticisms and Limitations

Theoretical Challenges

The nonlinear nature of the field equations in AQUAL, given by

\nabla \cdot \left[ \mu\left( \frac{|\nabla \phi|}{a_0} \right) \nabla \phi \right] = 4\pi G \rho

, prevents the superposition principle inherent to Newtonian gravity, making exact analytical solutions possible only in cases of high symmetry, such as spherical or planar configurations where the curl term vanishes. Beyond these, the theory relies on numerical methods, including multigrid solvers, to handle the computational complexity arising from the nonlinear interpolating function

\mu

. This nonlinearity also implies that the gravitational field from a composite system cannot be simply added from its components, complicating predictions for multi-body interactions. AQUAL lacks full Galilean invariance due to the presence of the fixed acceleration scale

a_0

, which defines a preferred frame where the theory's isotropy holds; boosts relative to this frame alter the form of the equations.^[23] However, in the deep-MOND limit (accelerations

\ll a_0

) and the Newtonian limit (accelerations

\gg a_0

), approximate invariance is restored, aligning with observed dynamics in those regimes. The theory faces tension with solar system precision tests, such as those from the Cassini mission constraining the gravitational quadrupole to near-Newtonian values, necessitating a specific form for the interpolating function

\nu(y) \approx 1 + \frac{1}{2} y

in the high-acceleration regime to match post-Newtonian parameters like

\gamma \approx 1

. This requirement for a sharp transition in

\nu(y)

or equivalent

\mu(x)

ensures minimal deviations from general relativity in strong-field environments while preserving MOND behavior at galactic scales.

Observational Constraints

On the scale of galaxy clusters, AQUAL significantly underpredicts the observed dynamics, as the modified gravitational acceleration fails to account for the full mass required to bind the systems without invoking an additional non-baryonic component often termed "phantom dark matter," which amounts to roughly 20-50% of the baryonic mass. For instance, in the Coma Cluster, hydrostatic equilibrium analyses of the intracluster gas indicate that AQUAL reproduces only about half the inferred total mass, necessitating this phantom matter or further modifications to the theory.^[24] These discrepancies highlight AQUAL's limitations in dense environments where the external field effect is weak, contrasting with its successes in isolated galactic rotation curves. Recent analyses of wide binary stars using Gaia DR3 data provide mixed empirical tests of AQUAL, particularly regarding the external field effect (EFE), which predicts that the gravitational anomaly weakens in the Solar Neighborhood's tidal field. Studies report a mild enhancement in relative velocities for separations beyond 0.1 pc, consistent with an EFE-modulated boost factor of approximately 1.4 in the deep-MOND regime as expected from AQUAL's nonlinear field equations, supporting MOND-like deviations from Newtonian predictions at accelerations around

10^{-10}

m/s².^[25] However, subsequent critiques reveal tensions, as refined sample selections and statistical treatments favor Newtonian dynamics or yield only marginal significance for the anomaly after accounting for contaminants like undetected tertiary companions, challenging AQUAL's deep-MOND predictions without additional refinements.^[26] These results suggest that while Gaia data offer tentative EFE support, they impose constraints requiring careful modeling of projection effects and selection biases to avoid overinterpreting the signal.^[27] As of 2025, updated analyses continue to debate the anomaly, with several studies favoring Newtonian gravity over MOND predictions.^[28] At cosmological scales, AQUAL encounters substantial difficulties in reproducing large-scale structure formation and the cosmic microwave background (CMB) power spectrum without supplementary fields or particles, as its non-relativistic formulation lacks a consistent framework for early-Universe perturbations and expansion history. Simulations incorporating AQUAL-like MOND gravity predict excessive power on small scales due to enhanced clustering in the nonlinear regime, leading to disagreements with observed matter power spectra from surveys like SDSS, where the theory overproduces structure by factors of up to 10 without dark matter or ad hoc scale-dependent adjustments.^[29] Similarly, AQUAL struggles with CMB anisotropies, failing to match the acoustic peak positions and damping tail observed by Planck without introducing additional relativistic degrees of freedom, as the theory's scalar field does not naturally generate the required primordial fluctuations or Silk damping effects. These issues underscore the need for full relativistic extensions beyond AQUAL to address cosmological observations coherently. In strong lensing and colliding cluster systems like the Bullet Cluster, AQUAL alone inadequately explains the spatial offset between baryonic gas and gravitational mass maps derived from lensing shear, as its non-relativistic nature cannot properly handle light deflection or collisionless dynamics without phantom matter, which traces baryons too closely to match the observed separation.^[30] Relativistic variants such as TeVeS can fit Bullet Cluster lensing data by adjusting vector and scalar field couplings, but this requires fine-tuning of parameters to separate lensing mass from intracluster medium centroids, with the predicted collision velocity being higher than observed unless further modifications are imposed.^[31] For AQUAL specifically, the absence of a tensor mode leads to failures in reproducing the lensing signal's amplitude, imposing tight constraints that favor hybrid models over the pure formulation.

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AQUAL

Background and History

Modified Newtonian Dynamics (MOND)

Development of AQUAL

Theoretical Formulation

Lagrangian Density

Nonlinear Field Equations

Relation to MOND and Key Features

Implementation of MOND Interpolation

Scale Invariance and External Field Effect

Predictions and Astrophysical Applications

Galaxy Rotation Curves

Baryonic Tully-Fisher Relation

Relativistic Extensions

Tensor-Vector-Scalar (TeVeS) Theory

Conservation Principles in Relativistic MOND

Criticisms and Limitations

Theoretical Challenges

Observational Constraints

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