Are we close to putting the anomalous perihelion precessions from Verlinde’s emergent gravity to the test?

Iorio, Lorenzo

doi:10.1140/epjc/s10052-017-4722-z

Cited by 13 publications

(21 citation statements)

References 34 publications

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“…Since the effect of dark mass is cumulative, a much larger effect is generated by galaxies and clusters of galaxies, and a preliminary discussion of that effect (that mimics dark matter) can be found in the original reference [1]. We point out that after the first version of this work several references have appeared [14], [15] that also discuss how to test Verlinde's emergent gravity.…”

Section: Discussionmentioning

confidence: 88%

“…The first integral was evaluated by assuming that the source and the observer are infinitely far from the star, which is for small lensing angles an excellent approximation. It is instructive to compare the first two contributions in (15).…”

Section: Gravitational Lensingmentioning

confidence: 99%

“…Due to the conical geometry, to a very good approximation that ray will exhibit an angle deflection of one half of the total deficit angle, i.e. The total deflection angle is then simply the sum of (15) and (16),…”

Section: Gravitational Lensingmentioning

confidence: 99%

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Gravitational microlensing in Verlinde's emergent gravity

Liu

Prokopec

2017

Physics Letters B

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We propose gravitational microlensing as a way of testing the emergent gravity theory recently proposed by Eric Verlinde~\cite{Verlinde:2016toy}. We consider two limiting cases: the dark mass of maximally anisotropic pressures (Case I) and of isotropic pressures (Case II). Our analysis of perihelion advancement of a planet shows that only Case I yields a viable theory. In this case the metric outside a star of mass $M_*$ can be modeled by that of a point-like global monopole whose mass is $M_*$ and a deficit angle $\Delta = \sqrt{(2GH_0M_*)/(3c^3)}$, where $H_0$ is the Hubble rate and $G$ the Newton constant. This deficit angle can be used to test the theory since light exhibits additional bending around stars given by, $\alpha_D\approx -\pi\Delta/2$. This angle is independent on the distance from the star and it affects equally light and massive particles. The effect is too small to be measurable today, but should be within reach of the next generation of high resolution telescopes. Finally we note that the advancement of periastron of a planet orbiting around a star or black hole, which equals $\pi\Delta$ per period, can be also used to test the theory.Comment: 19 pages, 2 figure

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Section: Discussionmentioning

confidence: 88%

Section: Gravitational Lensingmentioning

confidence: 99%

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Gravitational microlensing in Verlinde's emergent gravity

Liu

Prokopec

2017

Physics Letters B

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“…The full analytical expression of the Lense-Thirring periastron precession of a two-body system whose spin angular momenta are arbitrarily oriented in space is (Iorio 2017…”

Section: Using the Periastron Precessionmentioning

confidence: 99%

“…It is important to stress that, contrary to the periastron, neither the inclination nor the node undergo 1pN+2pN mass-dependent gravitoelectric shifts. Their full spin-orbit rates can be explicitly expressed as (Iorio 2017)…”

Section: The Spin-orbit Precessions Of the Inclination And The Nodementioning

confidence: 99%

The impact of the spin-orbit misalignment and of the spin of B on the Lense-Thrirring orbital precessions of the Double Pulsar PSR J0737-3039A/B

Iorio

2021

Preprint

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In the Double Pulsar, the Lense-Thirring periastron precession ωLT could be used to measure/constrain the moment of inertia I A of A. Conversely, if I A will be independently determined with sufficient accuracy by other means, tests of the Lense-Thirring effect could be performed. Such findings rely upon a formula for ωLT, A induced by the spin angular momentum S A of A, valid if the orbital angular momentum L and S A are aligned, and neglecting ωLT, B because of the smallness of S B . The impact on ωLT, A of the departures of the S A -L geometry from the ideal alignment is calculated. With the current upper bound on the misalignment angle δ A between them, the angles λ A , η A of S A are constrained within 85In units of the first order post-Newtonian mass-dependent periastron precession ωGR = 16.89 • yr −1 , a range variation ∆ ωLT, A ωLT, A max − ωLT, A min = 8 × 10 −8 ω GR is implied. The experimental uncertainty σ ωobs in measuring the periastron rate should become smaller by 2028-2030. Then, the spatial orientation of S B is constrained from the existing bounds on the misalignment angle δ B , and ωLT, B 2 × 10 −7 ωGR is correspondingly calculated. The error σ ωobs should become smaller around 2025. The Lense-Thirring inclination and node precessions İLT , ΩLT are predicted to be 0.05 arcseconds per year, far below the current experimental accuracies σ I obs = 0.5 • , σ Ω obs = 2 • in measuring I, Ω over 1.5 year with the scintillation technique. The Lense-Thirring rate ẋLT A of the projected semimajor axis x A of PSR J0737-3039A is 2 × 10 −16 s s −1 , just two orders of magnitude smaller than a putative experimental uncertainty σ ẋobs A 10 −14 s s −1 guessed from 2006 data.

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Fast particle-mesh code for Milgromian dynamics

Visser,

Eijt,

de Nijs

2024

A&A

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Modified Newtonian dynamics (MOND) is a promising alternative to dark matter. To further test the theory, there is a need for fluid- and particle-dynamics simulations. The force in MOND is not a direct particle-particle interaction, but derives from a potential for which a nonlinear partial differential equation (PDE) needs to be solved. Normally, this makes the problem of simulating dynamical evolution computationally expensive. We intend to develop a fast particle-mesh (PM) code for MOND (the AQUAL formalism). We transformed the nonlinear equation for MOND into a system of linear PDEs plus one algebraic equation. An iterative scheme with the fast Fourier transform (FFT) produces successively better numerical approximations. The algorithm was tested for dynamical systems in MOND where analytical solutions are known: the two-body problem, a body with a circular ring, and a spherical distribution of particles in thermal equilibrium in the self-consistent potential. The PM code can accurately calculate the forces at subpixel scale and reproduces the analytical solutions. Four iterations are required for the potential, but when the spatial steps are small compared to the kernel width, one iteration is suffices. The use of a smoothing kernel for the accelerations is inevitable in order to eliminate the self-gravity of the point particles. Our PDE solver is $15$ to $42$ times as slow as a standard Poisson solver. However, the smoothing and particle propagation takes up most of the time above one particle per $10^3$ pixels. The FFTs, the smoothing, and the propagation part in the code can all be parallelized.

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Are we close to putting the anomalous perihelion precessions from Verlinde’s emergent gravity to the test?

Cited by 13 publications

References 34 publications

Gravitational microlensing in Verlinde's emergent gravity

Gravitational microlensing in Verlinde's emergent gravity

The impact of the spin-orbit misalignment and of the spin of B on the Lense-Thrirring orbital precessions of the Double Pulsar PSR J0737-3039A/B

Fast particle-mesh code for Milgromian dynamics

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