Astronomy:Modified Newtonian dynamics
Modified Newtonian dynamics (MOND) is a hypothesis that proposes a modification of Newton's law of universal gravitation to account for observed properties of galaxies. It is an alternative to the hypothesis of dark matter in terms of explaining why galaxies do not appear to obey the currently understood laws of physics.
Created in 1982 and first published in 1983 by Israeli physicist Mordehai Milgrom,^{[1]} the hypothesis' original motivation was to explain why the velocities of stars in galaxies were observed to be larger than expected based on Newtonian mechanics. Milgrom noted that this discrepancy could be resolved if the gravitational force experienced by a star in the outer regions of a galaxy was proportional to the square of its centripetal acceleration (as opposed to the centripetal acceleration itself, as in Newton's second law) or alternatively, if gravitational force came to vary inversely linearly with radius (as opposed to the inverse square of the radius, as in Newton's law of gravity). In MOND, violation of Newton's laws occurs at extremely small accelerations, characteristic of galaxies yet far below anything typically encountered in the Solar System or on Earth.
Unsolved problem in physics:

MOND is an example of a class of theories known as modified gravity, and is an alternative to the hypothesis that the dynamics of galaxies are determined by massive, invisible dark matter halos. Since Milgrom's original proposal, proponents of MOND have claimed to successfully predict a variety of galactic phenomena that they state are difficult to understand as consequences of dark matter.^{[2]}^{[3]} However, MOND and its generalizations do not adequately account for observed properties of galaxy clusters, and no satisfactory cosmological model has been constructed from the hypothesis.
The accurate measurement of the speed of gravitational waves compared to the speed of light in 2017 ruled out many hypotheses which used modified gravity.^{[4]} However, both Milgrom's bimetric formulation of MOND and nonlocal MOND are compatible with this measurement.
Overview
Several independent observations point to the fact that the visible mass in galaxies and galaxy clusters is insufficient to account for their dynamics, when analyzed using Newton's laws. This discrepancy – known as the "missing mass problem" – was first identified for clusters by Swiss astronomer Fritz Zwicky in 1933 (who studied the Coma cluster),^{[6]}^{[7]} and subsequently extended to include spiral galaxies by the 1939 work of Horace Babcock on Andromeda.^{[8]}
These early studies were augmented and brought to the attention of the astronomical community in the 1960s and 1970s by the work of Vera Rubin at the Carnegie Institute in Washington, who mapped in detail the rotation velocities of stars in a large sample of spirals. While Newton's Laws predict that stellar rotation velocities should decrease with distance from the galactic centre, Rubin and collaborators found instead that they remain almost constant^{[9]} – the rotation curves are said to be "flat". This observation necessitates at least one of the following:
(1) There exists in galaxies large quantities of unseen matter which boosts the stars' velocities beyond what would be expected on the basis of the visible mass alone, or (2) Newton's Laws do not apply to galaxies.
Option (1) leads to the dark matter hypothesis; option (2) leads to MOND.
The basic premise of MOND is that while Newton's laws have been extensively tested in highacceleration environments (in the Solar System and on Earth), they have not been verified for objects with extremely low acceleration, such as stars in the outer parts of galaxies. This led Milgrom to postulate a new effective gravitational force law (sometimes referred to as "Milgrom's law") that relates the true acceleration of an object to the acceleration that would be predicted for it on the basis of Newtonian mechanics.^{[1]} This law, the keystone of MOND, is chosen to reproduce the Newtonian result at high acceleration but leads to different ("deepMOND") behavior at low acceleration:

[math]\displaystyle{ F_\text{N} = m \, \mu\!\!\left( \frac{a}{\, a_0 \,} \right)\, a ~. }[/math]
(
)

Here F_{N} is the Newtonian force, m is the object's (gravitational) mass, a is its acceleration, μ(x) is an asyet unspecified function (called the interpolating function), and a_{0} is a new fundamental constant which marks the transition between the Newtonian and deepMOND regimes. Agreement with Newtonian mechanics requires
 [math]\displaystyle{ \begin{align} \mu(x) \longrightarrow 1 && \text{ for } x \gg 1 \end{align} ~, }[/math]
and consistency with astronomical observations requires
 [math]\displaystyle{ \begin{align} \mu(x) \longrightarrow x && \text{ for } x \ll 1 \end{align} ~. }[/math]
Beyond these limits, the interpolating function is not specified by the hypothesis, although it is possible to weakly constrain it empirically.^{[10]}^{[11]} Two common choices are the "simple interpolating function":
 [math]\displaystyle{ \mu\!\!\left( \frac{a}{\, a_0 \,} \right) = \frac{1}{\; 1 + \frac{\, a_0 \,}{a} \;} ~, }[/math]
and the "standard interpolating function":
 [math]\displaystyle{ \mu\!\!\left( \frac{a}{\, a_0 \,} \right) = \sqrt{\frac{1}{\; 1 + \left( \frac{\, a_0 \,}{a} \right)^2 \;}~} ~. }[/math]
Thus, in the deepMOND regime (a ≪ a_{0}):
 [math]\displaystyle{ F_\text{N} = m \frac{\, a^2 \,}{\, a_0 \,} ~. }[/math]
Applying this to an object of mass m in circular orbit around a point mass M (a crude approximation for a star in the outer regions of a galaxy), we find:

[math]\displaystyle{ \frac{\, G M m \,}{r^2} = m \frac{\; \left( \frac{\,v^2\,}{r} \right)^2 \;}{a_0} \quad \Longrightarrow \quad v^4 = G M a_0 ~, }[/math]
(
)

that is, the star's rotation velocity is independent of r, its distance from the centre of the galaxy – the rotation curve is flat, as required. By fitting his law to rotation curve data, Milgrom found [math]\displaystyle{ \, a_0 \approx 1.2 \times 10^{10} \mathrm{ms}^{2} \, }[/math] to be optimal. This simple law is sufficient to make predictions for a broad range of galactic phenomena.
Milgrom's law can be interpreted in two different ways:
 One possibility is to treat it as a modification to Newton's second law, so that the force on an object is not proportional to the particle's acceleration a but rather to [math]\displaystyle{ \,\mu\!\left( \frac{a}{\, a_0 \,} \right) a \,. }[/math] In this case, the modified dynamics would apply not only to gravitational phenomena, but also those generated by other forces, for example electromagnetism.^{[12]}
 Alternatively, Milgrom's law can be viewed as leaving Newton's Second Law intact and instead modifying the inversesquare law of gravity, so that the true gravitational force on an object of mass m due to another of mass M is roughly of the form [math]\displaystyle{ \,\frac{\, G M m \,}{\mu\!\!\left( \frac{a}{a_0} \right) r^2} ~. }[/math] In this interpretation, Milgrom's modification would apply exclusively to gravitational phenomena.
By itself, Milgrom's law is not a complete and selfcontained physical theory, but rather an ad hoc empirically motivated variant of one of the several equations that constitute classical mechanics. Its status within a coherent nonrelativistic hypothesis of MOND is akin to Kepler's Third Law within Newtonian mechanics; it provides a succinct description of observational facts, but must itself be explained by more fundamental concepts situated within the underlying hypothesis. Several complete classical hypotheses have been proposed (typically along "modified gravity" as opposed to "modified inertia" lines), which generally yield Milgrom's law exactly in situations of high symmetry and otherwise deviate from it slightly. A subset of these nonrelativistic hypotheses have been further embedded within relativistic theories, which are capable of making contact with nonclassical phenomena (e.g., gravitational lensing) and cosmology.^{[13]} Distinguishing both theoretically and observationally between these alternatives is a subject of current research.
The majority of astronomers, astrophysicists, and cosmologists accept dark matter as the explanation for galactic rotation curves^{[14]} (based on general relativity, and hence Newtonian mechanics), and are committed to a dark matter solution of the missingmass problem. MOND, by contrast, is actively studied by only a handful of researchers.
The primary difference between supporters of ΛCDM and MOND is in the observations for which they demand a robust, quantitative explanation, and those for which they are satisfied with a qualitative account, or are prepared to leave for future work. Proponents of MOND emphasize predictions made on galaxy scales (where MOND enjoys its most notable successes) and believe that a cosmological model consistent with galaxy dynamics has yet to be discovered. Proponents of ΛCDM require high levels of cosmological accuracy (which concordance cosmology provides) and argue that a resolution of galaxyscale issues will follow from a better understanding of the complicated baryonic astrophysics underlying galaxy formation.^{[2]}^{[15]}
Observational evidence for MOND
Since MOND was specifically designed to produce flat rotation curves, these do not constitute evidence for the hypothesis, but every matching observation adds to support of the empirical law. Nevertheless, proponents claim that a broad range of astrophysical phenomena at the galactic scale are neatly accounted for within the MOND framework.^{[13]}^{[16]} Many of these came to light after the publication of Milgrom's original papers and are difficult to explain using the dark matter hypothesis. The most prominent are the following:
 In addition to demonstrating that rotation curves in MOND are flat, equation 2 provides a concrete relation between a galaxy's total baryonic mass (the sum of its mass in stars and gas) and its asymptotic rotation velocity. This predicted relation was called by Milgrom the massasymptotic speed relation (MASSR); its observational manifestation is known as the baryonic Tully–Fisher relation (BTFR),^{[17]} and is found to conform quite closely to the MOND prediction.^{[18]}
 Milgrom's law fully specifies the rotation curve of a galaxy given only the distribution of its baryonic mass. In particular, MOND predicts a far stronger correlation between features in the baryonic mass distribution and features in the rotation curve than does the dark matter hypothesis (since dark matter dominates the galaxy's mass budget and is conventionally assumed not to closely track the distribution of baryons). Such a tight correlation is claimed to be observed in several spiral galaxies, a fact which has been referred to as "Renzo's rule".^{[13]}
 Since MOND modifies Newtonian dynamics in an accelerationdependent way, it predicts a specific relationship between the acceleration of a star at any radius from the centre of a galaxy and the amount of unseen (dark matter) mass within that radius that would be inferred in a Newtonian analysis. This is known as the mass discrepancyacceleration relation, and has been measured observationally.^{[19]}^{[20]} One aspect of the MOND prediction is that the mass of the inferred dark matter go to zero when the stellar centripetal acceleration becomes greater than a_{0}, where MOND reverts to Newtonian mechanics. In dark matter hypothesis, it is a challenge to understand why this mass should correlate so closely with acceleration, and why there appears to be a critical acceleration above which dark matter is not required.^{[2]}
 Both MOND and dark matter halos stabilize disk galaxies, helping them retain their rotationsupported structure and preventing their transformation into elliptical galaxies. In MOND, this added stability is only available for regions of galaxies within the deepMOND regime (i.e., with a < a_{0}), suggesting that spirals with a > a_{0} in their central regions should be prone to instabilities and hence less likely to survive to the present day.^{[21]} This may explain the "Freeman limit" to the observed central surface mass density of spiral galaxies, which is roughly a_{0}/G.^{[22]} This scale must be put in by hand in dark matterbased galaxy formation models.^{[23]}
 Particularly massive galaxies are within the Newtonian regime (a > a_{0}) out to radii enclosing the vast majority of their baryonic mass. At these radii, MOND predicts that the rotation curve should fall as 1/r, in accordance with Kepler's Laws. In contrast, from a dark matter perspective one would expect the halo to significantly boost the rotation velocity and cause it to asymptote to a constant value, as in less massive galaxies. Observations of highmass ellipticals bear out the MOND prediction.^{[24]}^{[25]}
 In MOND, all gravitationally bound objects with a < a_{0} – regardless of their origin – should exhibit a mass discrepancy when analyzed using Newtonian mechanics, and should lie on the BTFR. Under the dark matter hypothesis, objects formed from baryonic material ejected during the merger or tidal interaction of two galaxies ("tidal dwarf galaxies") are expected to be devoid of dark matter and hence show no mass discrepancy. Three objects unambiguously identified as Tidal Dwarf Galaxies appear to have mass discrepancies in close agreement with the MOND prediction.^{[26]}^{[27]}^{[28]}
 Recent work has shown that many of the dwarf galaxies around the Milky Way and Andromeda are located preferentially in a single plane and have correlated motions. This suggests that they may have formed during a close encounter with another galaxy and hence be Tidal Dwarf Galaxies. If so, the presence of mass discrepancies in these systems constitutes further evidence for MOND. In addition, it has been claimed that a gravitational force stronger than Newton's (such as Milgrom's) is required for these galaxies to retain their orbits over time.^{[29]}
 In 2020, a group of astronomers analyzing data from the Spitzer Photometry and Accurate Rotation Curves (SPARC) sample together with estimates of the largescale external gravitational field from an allsky galaxy catalog, concluded that there was highly statistically significant evidence of violations of the strong equivalence principle in weak gravitational fields in the vicinity of rotationally supported galaxies.^{[30]} They observed an effect consistent with the external field effect of Modified Newtonian dynamics and inconsistent with tidal effects in the LambdaCDM model paradigm commonly known as the Standard Model of Cosmology.
 In a 2022 published survey of dwarf galaxies from the Fornax Deep Survey (FDS) catalogue, a group of astronomers and physicists conclude that 'observed deformations of dwarf galaxies in the Fornax Cluster and the lack of low surface brightness dwarfs towards its centre are incompatible with ΛCDM expectations but well consistent with MOND.'^{[31]}
Complete MOND hypotheses
Milgrom's law requires incorporation into a complete hypothesis if it is to satisfy conservation laws and provide a unique solution for the time evolution of any physical system. Each of the theories described here reduce to Milgrom's law in situations of high symmetry (and thus enjoy the successes described above), but produce different behavior in detail.
Nonrelativistic
The first hypothesis of MOND (dubbed AQUAL) was constructed in 1984 by Milgrom and Jacob Bekenstein.^{[32]} AQUAL generates MONDian behavior by modifying the gravitational term in the classical Lagrangian from being quadratic in the gradient of the Newtonian potential to a more general function. (AQUAL is an acronym for A QUAdratic Lagrangian.) In formulae:
 [math]\displaystyle{ \begin{align} \mathcal{L}_\text{Newton} &=  \frac{1}{8 \pi G} \cdot \\nabla \phi\^2 \\ [6pt] \mathcal{L}_\text{AQUAL} &=  \frac{1}{8 \pi G} \cdot a_0^2 F \left (\tfrac{\\nabla \phi\^2}{a_0^2} \right ) \end{align} }[/math]
where [math]\displaystyle{ \phi }[/math] is the standard Newtonian gravitational potential and F is a new dimensionless function. Applying the Euler–Lagrange equations in the standard way then leads to a nonlinear generalization of the Newton–Poisson equation:
 [math]\displaystyle{ \nabla\cdot\left[ \mu \left( \frac{\left\ \nabla\phi \right\}{a_0} \right) \nabla\phi\right] = 4\pi G \rho }[/math]
This can be solved given suitable boundary conditions and choice of F to yield Milgrom's law (up to a curl field correction which vanishes in situations of high symmetry).
An alternative way to modify the gravitational term in the lagrangian is to introduce a distinction between the true (MONDian) acceleration field a and the Newtonian acceleration field a_{N}. The Lagrangian may be constructed so that a_{N} satisfies the usual NewtonPoisson equation, and is then used to find a via an additional algebraic but nonlinear step, which is chosen to satisfy Milgrom's law. This is called the "quasilinear formulation of MOND", or QUMOND,^{[33]} and is particularly useful for calculating the distribution of "phantom" dark matter that would be inferred from a Newtonian analysis of a given physical situation.^{[13]}
Both AQUAL and QUMOND propose changes to the gravitational part of the classical matter action, and hence interpret Milgrom's law as a modification of Newtonian gravity as opposed to Newton's second law. The alternative is to turn the kinetic term of the action into a functional depending on the trajectory of the particle. Such "modified inertia" theories, however, are difficult to use because they are timenonlocal, require energy and momentum to be nontrivially redefined to be conserved, and have predictions that depend on the entirety of a particle's orbit.^{[13]}
Relativistic
In 2004, Jacob Bekenstein formulated TeVeS, the first complete relativistic hypothesis using MONDian behaviour.^{[34]} TeVeS is constructed from a local Lagrangian (and hence respects conservation laws), and employs a unit vector field, a dynamical and nondynamical scalar field, a free function and a nonEinsteinian metric in order to yield AQUAL in the nonrelativistic limit (low speeds and weak gravity). TeVeS has enjoyed some success in making contact with gravitational lensing and structure formation observations,^{[35]} but faces problems when confronted with data on the anisotropy of the cosmic microwave background,^{[36]} the lifetime of compact objects,^{[37]} and the relationship between the lensing and matter overdensity potentials.^{[38]}
Several alternative relativistic generalizations of MOND exist, including BIMOND and generalized EinsteinAether theories.^{[13]} There is also a relativistic generalization of MOND that assumes a Lorentztype invariance as the physical basis of MOND phenomenology.^{[39]}
The external field effect
In Newtonian mechanics, an object's acceleration can be found as the vector sum of the acceleration due to each of the individual forces acting on it. This means that a subsystem can be decoupled from the larger system in which it is embedded simply by referring the motion of its constituent particles to their centre of mass; in other words, the influence of the larger system is irrelevant for the internal dynamics of the subsystem. Since Milgrom's law is nonlinear in acceleration, MONDian subsystems cannot be decoupled from their environment in this way, and in certain situations this leads to behaviour with no Newtonian parallel. This is known as the "external field effect" (EFE),^{[1]} for which there exists observational evidence.^{[30]}
The external field effect is best described by classifying physical systems according to their relative values of a_{in} (the characteristic acceleration of one object within a subsystem due to the influence of another), a_{ex} (the acceleration of the entire subsystem due to forces exerted by objects outside of it), and a_{0}:
 [math]\displaystyle{ a_{\mathrm{in}} \gt a_0 }[/math] : Newtonian regime
 [math]\displaystyle{ a_{\mathrm{ex}} \lt a_{\mathrm{in}} \lt a_0 }[/math] : DeepMOND regime
 [math]\displaystyle{ a_{\mathrm{in}} \lt a_0 \lt a_{\mathrm{ex}} }[/math] : The external field is dominant and the behavior of the system is Newtonian.
 [math]\displaystyle{ a_{\mathrm{in}} \lt a_{\mathrm{ex}} \lt a_0 }[/math] : The external field is larger than the internal acceleration of the system, but both are smaller than the critical value. In this case, dynamics is Newtonian but the effective value of G is enhanced by a factor of a_{0}/a_{ex}.^{[40]}
The external field effect implies a fundamental break with the strong equivalence principle (but not necessarily the weak equivalence principle). The effect was postulated by Milgrom in the first of his 1983 papers to explain why some open clusters were observed to have no mass discrepancy even though their internal accelerations were below a_{0}. It has since come to be recognized as a crucial element of the MOND paradigm.
The dependence in MOND of the internal dynamics of a system on its external environment (in principle, the rest of the universe) is strongly reminiscent of Mach's principle, and may hint towards a more fundamental structure underlying Milgrom's law. In this regard, Milgrom has commented:^{[41]}
It has been long suspected that local dynamics is strongly influenced by the universe at large, ala Mach's principle, but MOND seems to be the first to supply concrete evidence for such a connection. This may turn out to be the most fundamental implication of MOND, beyond its implied modification of Newtonian dynamics and general relativity, and beyond the elimination of dark matter.
Indeed, the potential link between MONDian dynamics and the universe as a whole (that is, cosmology) is augmented by the observation that the value of a_{0} (determined by fits to internal properties of galaxies) is within an order of magnitude of cH_{0}, where c is the speed of light and H_{0} is the Hubble constant (a measure of the presentday expansion rate of the universe).^{[1]} It is also close to the acceleration rate of the universe, and hence the cosmological constant. However, as yet no full hypothesis has been constructed which manifests these connections in a natural way.
Responses and criticism
Dark matter explanation
While acknowledging that Milgrom's law provides a succinct and accurate description of a range of galactic phenomena, many physicists reject the idea that classical dynamics itself needs to be modified and attempt instead to explain the law's success by reference to the behavior of dark matter. Some effort has gone towards establishing the presence of a characteristic acceleration scale as a natural consequence of the behavior of cold dark matter halos,^{[42]}^{[43]} although Milgrom has argued that such arguments explain only a small subset of MOND phenomena.^{[44]} An alternative proposal is to modify the properties of dark matter (e.g., to make it interact strongly with itself or baryons) in order to induce the tight coupling between the baryonic and dark matter mass that the observations point to.^{[45]} Finally, some researchers suggest that explaining the empirical success of Milgrom's law requires a more radical break with conventional assumptions about the nature of dark matter. One idea (dubbed "dipolar dark matter") is to make dark matter gravitationally polarizable by ordinary matter and have this polarization enhance the gravitational attraction between baryons.^{[46]}
Outstanding problems for MOND
The most serious problem facing Milgrom's law is that it cannot eliminate the need for dark matter in all astrophysical systems: galaxy clusters show a residual mass discrepancy even when analyzed using MOND.^{[2]} The fact that some form of unseen mass must exist in these systems detracts from the adequacy of MOND as a solution to the missing mass problem, although the amount of extra mass required is a fifth that of a Newtonian analysis, and there is no requirement that the missing mass be nonbaryonic. It has been speculated that 2 eV neutrinos could account for the cluster observations in MOND while preserving the hypothesis's successes at the galaxy scale.^{[47]}^{[48]} Indeed, analysis of sharp lensing data for the galaxy cluster Abell 1689 shows that MOND only becomes distinctive at Mpc distance from the center, so that Zwicky's conundrum remains,^{[49]} and 1.8 eV neutrinos are needed in clusters.^{[50]}
The 2006 observation of a pair of colliding galaxy clusters known as the "Bullet Cluster",^{[51]} poses a significant challenge for all theories proposing a modified gravity solution to the missing mass problem, including MOND. Astronomers measured the distribution of stellar and gas mass in the clusters using visible and Xray light, respectively, and in addition mapped the inferred dark matter density using gravitational lensing. In MOND, one would expect the "missing mass" to be centred on regions of visible mass which experience accelerations lower than a_{0} (assuming the external field effect is negligible). In ΛCDM, on the other hand, one would expect the dark matter to be significantly offset from the visible mass because the halos of the two colliding clusters would pass through each other (assuming, as is conventional, that dark matter is collisionless), whilst the cluster gas would interact and end up at the centre. An offset is clearly seen in the observations. It has been suggested, however, that MONDbased models may be able to generate such an offset in strongly nonspherically symmetric systems, such as the Bullet Cluster.^{[52]}
A significant piece of evidence in favor of standard dark matter is the observed anisotropies in the cosmic microwave background.^{[53]} While ΛCDM is able to explain the observed angular power spectrum, MOND has a much harder time, though recently it has been shown that MOND can fit the observations too.^{[54]} MOND also encounters difficulties explaining structure formation, with density perturbations in MOND perhaps growing so rapidly that too much structure is formed by the present epoch.^{[55]} However, forming galaxies more rapidly than in ΛCDM can be a good thing to some extent.^{[56]}
Several other studies have noted observational difficulties with MOND. For example, it has been claimed that MOND offers a poor fit to the velocity dispersion profile of globular clusters and the temperature profile of galaxy clusters,^{[57]}^{[58]} that different values of a_{0} are required for agreement with different galaxies' rotation curves,^{[59]} and that MOND is naturally unsuited to forming the basis of cosmology.^{[60]} Furthermore, many versions of MOND predict that the speed of light is different to the speed of gravity, but in 2017 the speed of gravitational waves was measured to be equal to the speed of light to high precision.^{[4]} This is well understood in modern relativistic theories of MOND, with the constraint from gravitational waves actually helping by substantially restricting how a covariant theory might be constructed.^{[61]}
Besides these observational issues, MOND and its relativistic generalizations are plagued by theoretical difficulties.^{[60]}^{[62]} Several ad hoc and inelegant additions to general relativity are required to create a theory compatible with a nonNewtonian nonrelativistic limit, though the predictions in this limit are rather clear. This is the case for the more commonly used modified gravity versions of MOND, but some formulations (most prominently those based on modified inertia) have long suffered from poor compatibility with cherished physical principles such as conservation laws. Researchers working on MOND generally do not interpret it as a modification of inertia, with only very limited work done on this area.
Proposals for testing MOND
Several observational and experimental tests have been proposed to help distinguish^{[63]} between MOND and dark matterbased models:
 The detection of particles suitable for constituting cosmological dark matter would strongly suggest that ΛCDM is correct and no modification to Newton's laws is required.
 If MOND is taken as a theory of modified inertia, it predicts the existence of anomalous accelerations on the Earth at particular places and times of the year. These could be detected in a precision experiment. This prediction would not hold if MOND is taken as a theory of modified gravity, as the external field effect produced by the Earth would cancel MONDian effects at the Earth's surface.^{[64]}^{[65]}
 It has been suggested that MOND could be tested in the Solar System using the LISA Pathfinder mission (launched in 2015). In particular, it may be possible to detect the anomalous tidal stresses predicted by MOND to exist at the EarthSun saddlepoint of the Newtonian gravitational potential.^{[66]} It may also be possible to measure MOND corrections to the perihelion precession of the planets in the Solar System,^{[67]} or a purposebuilt spacecraft.^{[68]}
 One potential astrophysical test of MOND is to investigate whether isolated galaxies behave differently from otherwiseidentical galaxies that are under the influence of a strong external field. Another is to search for nonNewtonian behaviour in the motion of binary star systems where the stars are sufficiently separated for their accelerations to be below a_{0}.^{[69]}
 Testing MOND using the redshiftdependence of radial acceleration – Sabine Hossenfelder and Tobias Mistele propose a parameterfree MOND model they call Covariant Emergent Gravity and suggest that as measurements of radial acceleration improve, various MOND models and particle dark matter might be distinguishable because MOND predicts a much smaller redshiftdependence.^{[70]}
See also
 MOND researchers:
 Biography:Mordehai Milgrom – Israeli physicist
 Biography:Jacob Bekenstein – MexicanIsraeli physicist
 Astronomy:AQUAL – Theory of gravity
 Entropic gravity – Theory in modern physics that describes gravity as an entropic force
 Astronomy:Cold dark matter – Hypothetical type of dark matter in physics
 Astronomy:Dark matter – Hypothetical form of matter
 Astronomy:Tully–Fisher relation – Trend in astronomy
References
 ↑ ^{1.0} ^{1.1} ^{1.2} ^{1.3} Milgrom, M. (1983). "A modification of the Newtonian dynamics as a possible alternative to the hidden mass hypothesis". Astrophysical Journal 270: 365–370. doi:10.1086/161130. Bibcode: 1983ApJ...270..365M.. Milgrom, M. (1983). "A modification of the Newtonian dynamics  Implications for galaxies". Astrophysical Journal 270: 371–383. doi:10.1086/161131. Bibcode: 1983ApJ...270..371M.. Milgrom, M. (1983). "A modification of the Newtonian dynamics  Implications for galaxy systems". Astrophysical Journal 270: 384. doi:10.1086/161132. Bibcode: 1983ApJ...270..384M..
 ↑ ^{2.0} ^{2.1} ^{2.2} ^{2.3} McGaugh, S. (2015). "A Tale of Two Paradigms: the Mutual Incommensurability of LCDM and MOND". Canadian Journal of Physics 93 (2): 250–259. doi:10.1139/cjp20140203. Bibcode: 2015CaJPh..93..250M.
 ↑ Kroupa, P.; Pawlowski, M.; Milgrom, M. (2012). "The failures of the standard model of cosmology require a new paradigm". International Journal of Modern Physics D 21 (14): 1230003. doi:10.1142/S0218271812300030. Bibcode: 2012IJMPD..2130003K.
 ↑ ^{4.0} ^{4.1} Boran, Sibel; Desai, Shantanu; Kahya, Emre; Woodard, Richard (2018). "GW170817 Falsifies Dark Matter Emulators". Physical Review D 97 (4): 041501. doi:10.1103/PhysRevD.97.041501. Bibcode: 2018PhRvD..97d1501B.
 ↑ Data are from: Corbelli, E.; Salucci, P. (2000). "The extended rotation curve and the dark matter halo of M33". Monthly Notices of the Royal Astronomical Society 311 (2): 441–447. doi:10.1046/j.13658711.2000.03075.x. Bibcode: 2000MNRAS.311..441C.
 ↑ Zwicky, F. (1933). "Die Rotverschiebung von extragalaktischen Nebeln". Helvetica Physica Acta 6: 110–127. Bibcode: 1933AcHPh...6..110Z.
 ↑ Zwicky, F. (1937). "On the masses of nebulae and of clusters of nebulae". The Astrophysical Journal 86: 217. doi:10.1086/143864. Bibcode: 1937ApJ....86..217Z.
 ↑ Babcock, H. (1939). "The rotation of the Andromeda Nebula". Lick Observatory Bulletin 498 (498): 41. doi:10.5479/ADS/bib/1939LicOB.19.41B. Bibcode: 1939LicOB..19...41B.
 ↑ Rubin, Vera C.; Ford, W. Kent, Jr. (February 1970). "Rotation of the Andromeda Nebula from a spectroscopic survey of emission regions". The Astrophysical Journal 159: 379–403. doi:10.1086/150317. Bibcode: 1970ApJ...159..379R.
 ↑ Gentile, G.; Famaey, B.; de Blok, W.J.G. (2011). "THINGS about MOND". Astronomy & Astrophysics 527 (A76): A76. doi:10.1051/00046361/201015283. Bibcode: 2011A&A...527A..76G.
 ↑ Famaey, B.; Binney, J. (2005). "Modified Newtonian dynamics in the Milky Way". Monthly Notices of the Royal Astronomical Society 363 (2): 603–608. doi:10.1111/j.13652966.2005.09474.x. Bibcode: 2005MNRAS.363..603F.
 ↑ Milgrom, M. (2011). "MOND – Particularly as modified inertia". Acta Physica Polonica B 42 (11): 2175. doi:10.5506/APhysPolB.42.2175.
 ↑ ^{13.0} ^{13.1} ^{13.2} ^{13.3} ^{13.4} ^{13.5} Famaey, B.; McGaugh, S. (2012). "Modified Newtonian dynamics (MOND): Observational phenomenology and relativistic extensions". Living Reviews in Relativity 15 (1): 10. doi:10.12942/lrr201210. PMID 28163623. Bibcode: 2012LRR....15...10F.
 ↑ Kroupa, Pavel (18 November 2013). The vast polar structures around the Milky Way and Andromeda (video). Archived from the original on 20211215 – via YouTube. Kroupa asserts that the majority opinion is wrong, and that empirical evidence rules out the ΛCDM model.
 ↑ Sanders, R.H. (2014). "A historical perspective on modified Newtonian dynamics". Canadian Journal of Physics 93 (2): 126–138. doi:10.1139/cjp20140206. Bibcode: 2015CaJPh..93..126S.
 ↑ Milgrom, Mordehai (2014). "MOND laws of galactic dynamics". Monthly Notices of the Royal Astronomical Society 437 (3): 2531–2541. doi:10.1093/mnras/stt2066. Bibcode: 2014MNRAS.437.2531M.
 ↑ McGaugh, S. S.; Schombert, J. M.; Bothun, G. D.; De Blok, W. J. G. (2000). "The Baryonic TullyFisher Relation". The Astrophysical Journal 533 (2): L99–L102. doi:10.1086/312628. PMID 10770699. Bibcode: 2000ApJ...533L..99M.
 ↑ McGaugh, Stacy S. (2012). "The Baryonic TullyFisher Relation of GasRich Galaxies as a Test of Λcdm and Mond". The Astronomical Journal 143 (2): 40. doi:10.1088/00046256/143/2/40. Bibcode: 2012AJ....143...40M.
 ↑ R. Sanders, "Mass discrepancies in galaxies: dark matter and alternatives", The Astronomy and Astrophysics Review 1990, Volume 2, Issue 1, pp 128
 ↑ McGaugh, Stacy S. (2004). "The Mass Discrepancy–Acceleration Relation: Disk Mass and the Dark Matter Distribution". The Astrophysical Journal 609 (2): 652–666. doi:10.1086/421338. Bibcode: 2004ApJ...609..652M.
 ↑ Jiménez, M. A.; Hernandez, X. (2014). "Disk stability under MONDian gravity". arXiv:1406.0537 [astroph.GA].
 ↑ McGaugh, S. (1998). "Testing the Hypothesis of Modified Dynamics with Low Surface Brightness Galaxies and Other Evidence". Astrophys J 499 (1): 66–81. doi:10.1086/305629. Bibcode: 1998ApJ...499...66M.
 ↑ McGaugh, S. (2005). "Balance of Dark and Luminous Mass in Rotating Galaxies". Phys. Rev. Lett. 95 (17): 171302. doi:10.1103/physrevlett.95.171302. PMID 16383816. Bibcode: 2005PhRvL..95q1302M.
 ↑ Romanowsky, A.J.; Douglas, N.G.; Arnaboldi, M.; Kuijken, K.; Merrifield, M.R.; Napolitano, N.R.; Capaccioli, M.; Freeman, K.C. (2003). "A Dearth of Dark Matter in Ordinary Elliptical Galaxies". Science 301 (5640): 1696–1698. doi:10.1126/science.1087441. PMID 12947033. Bibcode: 2003Sci...301.1696R.</
 ↑ Milgrom, M.; Sanders, R.H. (2003). "Modified Newtonian Dynamics and the 'Dearth of Dark Matter in Ordinary Elliptical Galaxies'". Astrophys J 599 (1): 25–28. doi:10.1086/381138. Bibcode: 2003ApJ...599L..25M.
 ↑ Bournaud, F.; Duc, P.A.; Brinks, E.; Boquien, M.; Amram, P.; Lisenfeld, U.; Koribalski, B. S.; Walter, F. et al. (2007). "Missing Mass in Collisional Debris from Galaxies". Science 316 (5828): 1166–1169. doi:10.1126/science.1142114. PMID 17495138. Bibcode: 2007Sci...316.1166B.
 ↑ Gentile, G.; Famaey, B.; Combes, F.; Kroupa, P.; Zhao, H. S.; Tiret, O. (2007). "Tidal dwarf galaxies as a test of fundamental physics". Astronomy & Astrophysics 472 (2): L25–L28. doi:10.1051/00046361:20078081. Bibcode: 2007A&A...472L..25G.
 ↑ Kroupa, P. (2012). "The Dark Matter Crisis: Falsification of the Current Standard Model of Cosmology". Publications of the Astronomical Society of Australia 29 (4): 395–433. doi:10.1071/AS12005. Bibcode: 2012PASA...29..395K.
 ↑ Kroupa, Pavel (2015). "Lessons from the Local Group (And Beyond) on Dark Matter". Lessons from the Local Group. pp. 337–352. doi:10.1007/9783319106144_28. ISBN 9783319106137.
 ↑ ^{30.0} ^{30.1} Chae, KyuHyun; Lelli, Federico; Desmond, Harry; McGaugh, Stacy S.; Li, Pengfei; Schombert, James M. (2020). "Testing the Strong Equivalence Principle: Detection of the External Field Effect in Rotationally Supported Galaxies". The Astrophysical Journal 904 (1): 51. doi:10.3847/15384357/abbb96. Bibcode: 2020ApJ...904...51C.
 ↑ Asencio, Elena; Banik, Indranil; Mieske, Steffen; Venhola, Aku; Kroupa, Pavel; Zhao, Hongsheng (2022). "The distribution and morphologies of Fornax Cluster dwarf galaxies suggest they lack dark matter". Monthly Notices of the Royal Astronomical Society 515 (2): 2981–3013. doi:10.1093/mnras/stac1765.
 ↑ Jacob Bekenstein; M. Milgrom (1984). "Does the missing mass problem signal the breakdown of Newtonian gravity?". Astrophys. J. 286: 7–14. doi:10.1086/162570. Bibcode: 1984ApJ...286....7B.
 ↑ Milgrom, Mordehai (2010). "Quasilinear formulation of MOND". Monthly Notices of the Royal Astronomical Society 403 (2): 886–895. doi:10.1111/j.13652966.2009.16184.x. Bibcode: 2010MNRAS.403..886M.
 ↑ Jacob D. Bekenstein (2004). "Relativistic gravitation theory for the MOND paradigm". Phys. Rev. D70 (8): 83509. doi:10.1103/PhysRevD.70.083509. Bibcode: 2004PhRvD..70h3509B.
 ↑ Clifton, Timothy; Ferreira, Pedro G.; Padilla, Antonio; Skordis, Constantinos (2012). "Modified gravity and cosmology". Physics Reports 513 (1–3): 1–189. doi:10.1016/j.physrep.2012.01.001. Bibcode: 2012PhR...513....1C.
 ↑ Slosar, Anže; Melchiorri, Alessandro; Silk, Joseph I. (2005). "Test of modified Newtonian dynamics with recent Boomerang data". Physical Review D 72 (10): 101301. doi:10.1103/PhysRevD.72.101301. Bibcode: 2005PhRvD..72j1301S.
 ↑ Seifert, M. D. (2007). "Stability of spherically symmetric solutions in modified theories of gravity". Physical Review D 76 (6): 064002. doi:10.1103/PhysRevD.76.064002. Bibcode: 2007PhRvD..76f4002S.
 ↑ Zhang, P.; Liguori, M.; Bean, R.; Dodelson, S. (2007). "Probing Gravity at Cosmological Scales by Measurements which Test the Relationship between Gravitational Lensing and Matter Overdensity". Physical Review Letters 99 (14): 141302. doi:10.1103/PhysRevLett.99.141302. PMID 17930657. Bibcode: 2007PhRvL..99n1302Z.
 ↑ Alzain, Mohammed (2017). "Modified Newtonian Dynamics (MOND) as a Modification of Newtonian Inertia". Journal of Astrophysics and Astronomy 38 (4): 59. doi:10.1007/s1203601794790. Bibcode: 2017JApA...38...59A.
 ↑ S. McGaugh, The EFE in MOND
 ↑ Milgrom, Mordehai (2008). "The MOND paradigm". arXiv:0801.3133 [astroph].
 ↑ Kaplinghat, Manoj; Turner, Michael (2002). "How Cold Dark Matter Theory Explains Milgrom's Law". The Astrophysical Journal 569 (1): L19–L22. doi:10.1086/340578. Bibcode: 2002ApJ...569L..19K.
 ↑ Blake, Chris; James, J. Berian; Poole, Gregory B. (2014). "Using the topology of largescale structure in the WiggleZ Dark Energy Survey as a cosmological standard ruler". Monthly Notices of the Royal Astronomical Society 437 (3): 2488–2506. doi:10.1093/mnras/stt2062. Bibcode: 2014MNRAS.437.2488B.
 ↑ Milgrom, Mordehai (2002). "Do Modified Newtonian Dynamics Follow from the Cold Dark Matter Paradigm?". The Astrophysical Journal 571 (2): L81–L83. doi:10.1086/341223. Bibcode: 2002ApJ...571L..81M.
 ↑ J. Bullock (2014), SelfInteracting Dark Matter
 ↑ Blanchet, Luc (2007). "Gravitational polarization and the phenomenology of MOND". Classical and Quantum Gravity 24 (14): 3529–3539. doi:10.1088/02649381/24/14/001. Bibcode: 2007CQGra..24.3529B.
 ↑ Angus, Garry W.; Shan, Huan Yuan; Zhao, Hong Sheng; Famaey, Benoit (2007). "On the Proof of Dark Matter, the Law of Gravity, and the Mass of Neutrinos". The Astrophysical Journal Letters 654 (1): L13–L16. doi:10.1086/510738. Bibcode: 2007ApJ...654L..13A.
 ↑ R.H. Sanders (2007). "Neutrinos as cluster dark matter". Monthly Notices of the Royal Astronomical Society 380 (1): 331–338. doi:10.1111/j.13652966.2007.12073.x. Bibcode: 2007MNRAS.380..331S.
 ↑ Nieuwenhuizen, Theodorus M. (2016). "How Zwicky already ruled out modified gravity theories without dark matter". Fortschritte der Physik 65 (6–8): 1600050. doi:10.1002/prop.201600050.
 ↑ Nieuwenhuizen, Theodorus M. (2015). "Dirac neutrino mass from a neutrino dark matter model for the galaxy cluster Abell 1689". Journal of Physics: Conference Series 701 (1): 012022(13pp). doi:10.1088/17426596/701/1/012022. Bibcode: 2016JPhCS.701a2022N.
 ↑ Clowe, Douglas; Bradač, Maruša; Gonzalez, Anthony H.; Markevitch, Maxim; Randall, Scott W.; Jones, Christine; Zaritsky, Dennis (2006). "A Direct Empirical Proof of the Existence of Dark Matter". The Astrophysical Journal Letters 648 (2): L109–L113. doi:10.1086/508162. Bibcode: 2006ApJ...648L.109C.
 ↑ G.W. Angus; B. Famaey; H. Zhao (September 2006). "Can MOND take a bullet? Analytical comparisons of three versions of MOND beyond spherical symmetry". Mon. Not. R. Astron. Soc. 371 (1): 138–146. doi:10.1111/j.13652966.2006.10668.x. Bibcode: 2006MNRAS.371..138A.
 ↑ See Dark matter.
 ↑ Constantinos Skordis; Tom Zlosnik (2021). "New Relativistic Theory for Modified Newtonian Dynamics". Physical Review Letters 127 (16): 161302. doi:10.1103/PhysRevLett.127.161302. Bibcode: 2021PhRvL.127p1302S.
 ↑ McGaugh, Stacy (2015). "A tale of two paradigms: The mutual incommensurability of ΛCDM and MOND". Canadian Journal of Physics 93 (2): 250–259. doi:10.1139/cjp20140203. Bibcode: 2015CaJPh..93..250M.
 ↑ Charles L. Steinhardt; Peter Capak; Dan Masters; Josh S. Speagle (2016). "The Impossibly Early Galaxy Problem". The Astrophysical Journal 824 (1): 21. doi:10.3847/0004637X/824/1/21. Bibcode: 2016ApJ...824...21S.
 ↑ Charles Seife (2004). Alpha and Omega. Penguin Books. pp. 100–101. ISBN 0142004464. https://archive.org/details/alphaomegasearch0000seif. "Modified Newtonian dynamics."
 ↑ Anthony Aguirre; Joop Schaye; Eliot Quataert (2001). "Problems for Modified Newtonian Dynamics in Clusters and the Lyα Forest?". The Astrophysical Journal 561 (2): 550–558. doi:10.1086/323376. Bibcode: 2001ApJ...561..550A.
 ↑ S. M. Kent, "Dark matter in spiral galaxies. II  Galaxies with H I rotation curves", 1987, AJ, 93, 816
 ↑ ^{60.0} ^{60.1} Scott, D.; White, M.; Cohn, J. D.; Pierpaoli, E. (2001). "Cosmological Difficulties with Modified Newtonian Dynamics (or: La Fin du MOND?)". arXiv:astroph/0104435.
 ↑ Constantinos Skordis; Tom Zlosnik (2019). "New Relativistic Theory for Modified Newtonian Dynamics". Physical Review D 100 (10): 104013. doi:10.1103/PhysRevD.100.104013. Bibcode: 2019PhRvD.100j4013S.
 ↑ Contaldi, Carlo R.; Wiseman, Toby; Withers, Benjamin (2008). "TeVeS gets caught on caustics". Physical Review D 78 (4): 044034. doi:10.1103/PhysRevD.78.044034. Bibcode: 2008PhRvD..78d4034C.
 ↑ Wallin, John F.; Dixon, David S.; Page, Gary L. (23 May 2007). "Testing Gravity in the Outer Solar System: Results from TransNeptunian Objects". The Astrophysical Journal 666 (2): 1296–1302. doi:10.1086/520528. Bibcode: 2007ApJ...666.1296W.
 ↑ Ignatiev, A.Yu. (2015). "Testing MOND on Earth". Canadian Journal of Physics 93 (2): 166–168. doi:10.1139/cjp20140164. Bibcode: 2015CaJPh..93..166I.
 ↑ De Lorenci, V. A.; FaúndezAbans, M.; Pereira, J. P. (2009). "Testing the Newton second law in the regime of small accelerations". Astronomy & Astrophysics 503 (1): L1–L4. doi:10.1051/00046361/200811520. Bibcode: 2009A&A...503L...1D.
 ↑ Trenkel, Christian; Kemble, Steve; Bevis, Neil; Magueijo, Joao (2010). "Testing MOND/TEVES with LISA Pathfinder". arXiv:1001.1303 [astroph.CO].
 ↑ Blanchet, Luc; Novak, Jerome (2011). "Testing MOND in the Solar System". arXiv:1105.5815 [astroph.CO].
 ↑ Sahni, Varun; Shtanov, Yuri (2008). "Apsis: An Artificial Planetary System in Space to Probe ExtraDimensional Gravity and Mond". International Journal of Modern Physics D 17 (3n04): 453–466. doi:10.1142/S0218271808012127. Bibcode: 2008IJMPD..17..453S.
 ↑ Hernandez, X.; Jiménez, M. A.; Allen, C. (2012). "Wide binaries as a critical test of classical gravity". The European Physical Journal C 72 (2): 1884. doi:10.1140/epjc/s1005201218846. Bibcode: 2012EPJC...72.1884H.
 ↑ Hossenfelder, Sabine; Mistele, Tobias (2018). "The redshiftdependence of radial acceleration: Modified gravity versus particle dark matter". International Journal of Modern Physics D 27 (14). doi:10.1142/S0218271818470107. Bibcode: 2018IJMPD..2747010H.
Further reading
Technical:
 Merritt, David (2020). A Philosophical Approach to MOND: Assessing the Milgromian Research Program in Cosmology (Cambridge: Cambridge University Press ), 282 pp. ISBN:9781108492690
 Milgrom, Mordehai (2014). "The MOND paradigm of modified dynamics". Scholarpedia 9 (6): 31410. doi:10.4249/scholarpedia.31410. Bibcode: 2014SchpJ...931410M.
 Famaey, Benoît; McGaugh, Stacy S. (2012). "Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions". Living Reviews in Relativity 15 (1): 10. doi:10.12942/lrr201210. PMID 28163623. Bibcode: 2012LRR....15...10F.
 McGaugh, Stacy S. (2015). "A tale of two paradigms: The mutual incommensurability of ΛCDM and MOND". Canadian Journal of Physics 93 (2): 250–259. doi:10.1139/cjp20140203. Bibcode: 2015CaJPh..93..250M.
 Milgrom, Mordehai (2015). "MOND theory". Canadian Journal of Physics 93 (2): 107–118. doi:10.1139/cjp20140211. Bibcode: 2015CaJPh..93..107M.
 Kroupa, Pavel (2015). "Galaxies as simple dynamical systems: Observational data disfavor dark matter and stochastic star formation". Canadian Journal of Physics 93 (2): 169–202. doi:10.1139/cjp20140179. Bibcode: 2015CaJPh..93..169K.
 Clifton, Timothy; Ferreira, Pedro G.; Padilla, Antonio; Skordis, Constantinos (2012). "Modified gravity and cosmology". Physics Reports 513 (1–3): 1–189. doi:10.1016/j.physrep.2012.01.001. Bibcode: 2012PhR...513....1C.
 Mannheim, P. (2006). "Alternatives to dark matter and dark energy". Progress in Particle and Nuclear Physics 56 (2): 340–445. doi:10.1016/j.ppnp.2005.08.001. Bibcode: 2006PrPNP..56..340M.
Popular:
 A nonStandard model, David Merritt, Aeon Magazine, July 2021
 Dark matter critics focus on details, ignore big picture, Lee, 14 Nov 2012
 Milgrom, Mordehai (2009). "MOND: Time for a change of mind?". arXiv:0908.3842 [astroph.CO].
 "Dark matter" doubters not silenced yet, World Science, 2 Aug 2007
 Does Dark Matter Really Exist?, Milgrom, Scientific American, Aug 2002
External links
 The MOND pages, Stacy McGaugh
 Mordehai Milgrom's website
 "The Dark Matter Crisis" blog, Pavel Kroupa, Marcel Pawlowski
 Pavel Kroupa's website
 Hossenfelder, Sabine (1 Feb 2016). "The superfluid Universe". https://aeon.co/essays/isdarkmattersubatomicparticlesasuperfluidorboth. Superfluid dark matter may provide a more natural way to arrive at the MOND equation.
Original source: https://en.wikipedia.org/wiki/Modified Newtonian dynamics.
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