Loss of Mass and Stability of Galaxies in Modified Newtonian Dynamics

Wu, Xufen; Zhao, Hongsheng; Famaey, Benoît; Gentile, Gianfranco; Tiret, O.; Combes, F.; Angus, Garry W.; Robin, A. C.

doi:10.1086/521103

Cited by 58 publications

(95 citation statements)

References 35 publications

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“…The EFE allows high-velocity stars to escape from the potential of the Milky Way Wu et al 2007) and implies that rotation curves of spiral galaxies should fall where the internal acceleration becomes equal to the external acceleration (Gentile et al 2007;Wu et al 2008).…”

Section: External Field Effect In Mondmentioning

confidence: 99%

“…One way to solve Eq. (1) is then to assume that the total acceleration is the sum of the internal a i and the external a e acceleration, which both satisfy the modified Poisson equation as (Bekenstein & Milgrom 1984;Wu et al 2007Wu et al , 2008Angus 2008)…”

Section: External Field Effect In Mondmentioning

confidence: 99%

“…Several attempts have been made considering the EFE. Wu et al (2007) simulated an isolated object with a static MONDian potential solver, but changed the boundary condition on the outermost grid point to be nonzero. Famaey et al (2007) estimated the escape velocity of galaxies in MOND and assumed μ(|a e + a i |/a 0 )a i = a N .…”

Section: External Field Effect In Mondmentioning

confidence: 99%

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Distant star clusters of the Milky Way in MOND

Haghi

Baumgardt

Kroupa³

2011

A&A

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We determine the mean velocity dispersion of six Galactic outer halo globular clusters, AM 1, Eridanus, Pal 3, Pal 4, Pal 15, and Arp 2 in the weak acceleration regime to test classical vs. modified Newtonian dynamics (MOND). Owing to the nonlinearity of MOND's Poisson equation, beyond tidal effects, the internal dynamics of clusters is affected by the external field in which they are immersed. For the studied clusters, particle accelerations are much lower than the critical acceleration a 0 of MOND, but the motion of stars is neither dominated by internal accelerations (a i a e ) nor external accelerations (a e a i ). We use the N-body code N-MODY in our analysis, which is a particle-mesh-based code with a numerical MOND potential solver developed by Ciotti et al. (2006, ApJ, 640, 741) to derive the line-of-sight velocity dispersion by adding the external field effect. We show that Newtonian dynamics predicts a low-velocity dispersion for each cluster, while in modified Newtonian dynamics the velocity dispersion is much higher. We calculate the minimum number of measured stars necessary to distinguish between Newtonian gravity and MOND with the Kolmogorov-Smirnov test. We also show that for most clusters it is necessary to measure the velocities of between 30 to 80 stars to distinguish between both cases. Therefore the observational measurement of the line-of-sight velocity dispersion of these clusters will provide a test for MOND.

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Section: External Field Effect In Mondmentioning

confidence: 99%

Section: External Field Effect In Mondmentioning

confidence: 99%

Section: External Field Effect In Mondmentioning

confidence: 99%

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Distant star clusters of the Milky Way in MOND

Haghi

Baumgardt

Kroupa³

2011

A&A

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“…observed phenomena in light of MOND Wu et al 2007Wu et al , 2008. Now let us suppose that the experimental details were provided and the experiment is ready to run.…”

Section: An Alternative Experimental Setupmentioning

confidence: 99%

Testing the Newton second law in the regime of small accelerations

Lorenci

Faúndez-Abans²,

Pereira

2009

A&A

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It has been pointed out that the Newtonian second law can be tested in the very small acceleration regime by using the combined movement of the Earth and Sun around the Galactic center of mass. It has been shown that there are only two brief intervals during the year in which the experiment can be completed, which correspond to only two specific spots on the Earth surface. An alternative experimental setup is presented to allow the measurement to be made on Earth at any location and at any time.

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“…Over the years, numerical schemes or solvers have been developed to solve the Poisson equation of less symmetric systems (see, e.g., Brada & Milgrom 1999;Ciotti et al 2006;Nipoti et al 2007a;Tiret & Combes 2007;Feix et al 2008;Llinares et al 2008;Londrillo & Nipoti 2009;Angus et al 2012;Candlish et al 2015;Lüghausen et al 2015). These codes enable us to study, in the framework of MOND, the structure and evolution of stellar systems (mostly accompanied by an N-Body code), such as stellar dynamics (see, e.g., Nipoti et al 2008Nipoti et al , 2011, disk galaxies (see, e.g., Brada & Milgrom 1999, 2000aTiret & Combes 2007Angus et al 2012;Lüghausen et al 2015), elliptical galaxies (see, e.g., Ciotti et al 2006;Nipoti et al 2007a;Wang et al 2008;Wu et al 2009), satellite galaxies with an external field effect (see, e.g., Brada & Milgrom 2000b;Nipoti et al 2007b;Wu et al 2007;Haghi et al 2011;Angus et al 2014;Lüghausen et al 2014;Candlish et al 2015), gravitational lensing (see, e.g., Feix et al 2008), and cosmic structure formation (see, e.g., Llinares et al 2008).…”

Section: Introductionmentioning

confidence: 99%

On the Problem of Deformed Spherical Systems in Modified Newtonian Dynamics

2016

ApJ

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Based on Newtonian dynamics, observations show that the luminous masses of astrophysical objects that are the size of a galaxy or larger are not enough to generate the measured motions which they supposedly determine. This is typically attributed to the existence of dark matter, which possesses mass but does not radiate (or absorb radiation). Alternatively, the mismatch can be explained if the underlying dynamics is not Newtonian. Within this conceptual scheme, Modified Newtonian Dynamics (MOND) is a successful theoretical paradigm. MOND is usually expressed in terms of a nonlinear Poisson equation, which is difficult to analyze for arbitrary matter distributions. We study the MONDian gravitational field generated by slightly non-spherically symmetric mass distributions based on the fact that both Newtonian and MONDian fields are conservative (which we refer to as the compatibility condition). As the non-relativistic version of MOND has two different formulations (AQUAL and QuMOND) and the compatibility condition can be expressed in two ways, there are four approaches to the problem in total. The method involves solving a suitably defined linear deformation potential, which generally depends on the choice of MOND interpolation function. However, for some specific form of the deformation potential, the solution is independent of the interpolation function.

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Loss of Mass and Stability of Galaxies in Modified Newtonian Dynamics

Cited by 58 publications

References 35 publications

Distant star clusters of the Milky Way in MOND

Distant star clusters of the Milky Way in MOND

Testing the Newton second law in the regime of small accelerations

On the Problem of Deformed Spherical Systems in Modified Newtonian Dynamics

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