Cosmological perturbations on local systems

Adkins, Gregory S.; McDonnell, Jordan; Fell, Richard N.

doi:10.1103/physrevd.75.064011

Cited by 71 publications

(110 citation statements)

References 35 publications

(47 reference statements)

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“…In the same publication, we will constrain the parameters α and n, taking into account the recent data of the ephemerides of the Solar System provided by INPOP10a [31,32] and EPM2011 [33][34][35]. Actually, perturbations in the form of power-law are present in different models of modified gravity, and their impact on the Solar System dynamics has been analyzed, for instance, in [36][37][38].…”

Section: Discussionmentioning

confidence: 99%

Weak-field spherically symmetric solutions inf(T)gravity

2015

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We study weak-field solutions having spherical symmetry in f (T ) gravity; to this end, we solve the field equations for a non diagonal tetrad, starting from Lagrangian in the form f (T ) = T +αT n , where α is a small constant, parameterizing the departure of the theory from GR. We show that the classical spherically symmetric solutions of GR, i.e. the Schwarzschild and Schwarzschild-de Sitter solutions, are perturbed by terms in the form ∝ r 2−2n and discuss the impact of these perturbations in observational tests. * Electronic address: matteo.ruggiero@polito.it † Electronic address: ninfa.radicella@sa.infn.it

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Section: Discussionmentioning

confidence: 99%

Weak-field spherically symmetric solutions inf(T)gravity

2015

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“…All the other potentials are power law functions of r . Perihelion precession for such kind of potentials were calculated in, e.g., [59][60][61]. For a potential V (r ) in the form V (r ) = γ r λ , it is found that the extra perihelion precession per orbital period is…”

Section: Perihelion Precessionmentioning

confidence: 99%

Solar system tests for realistic f(T) models with non-minimal torsion–matter coupling

Lin

Zhai

2017

Eur. Phys. J. C

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In the previous paper, we have constructed two f (T ) models with non-minimal torsion-matter coupling extension, which are successful in describing the evolution history of the Universe including the radiation-dominated era, the matter-dominated era, and the present accelerating expansion. Meantime, the significant advantage of these models is that they could avoid the cosmological constant problem of CDM. However, the non-minimal coupling between matter and torsion will affect the tests of the Solar system. In this paper, we study the effects of the Solar system in these models, including the gravitation redshift, geodetic effect and perihelion precession. We find that Model I can pass all three of the Solar system tests. For Model II, the parameter is constrained by the uncertainties of the planets' estimated perihelion precessions.

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“…Another potential source of major systematic uncertainty is represented by the N-body perturbations due to the other planets, especially Jupiter and Saturn. We will, now, demonstrate that, luckily, they can be modeled with sufficiently 2 Park et al [29] use the symbol for the in-plane, unbroken angle ω + cos I . high accuracy.…”

Section: The Perihelion Precessions Of the Planets Of The Solar Systemmentioning

confidence: 99%

“…Moreover, Eq. (4) is a distinctive feature of the modified model of gravity considered here which would be of great help, in principle, in discriminating Verlinde's theory from the anomalous precessions due to other more or less viable alternative models [1,2,14] by taking, e.g., the ratio of the perihelion rates for a pair of planets [14,15]. Table 1 The column˙ theo collects the theoretically predicted perihelion precessions, calculated for some planets of the Solar System according to Eq.…”

Section: Introductionmentioning

confidence: 99%

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

Iorio

2017

Eur. Phys. J. C

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In the framework of the emergent gravity scenario by Verlinde, it was recently observed by Liu and Prokopec that, among other things, an anomalous pericenter precession would affect the orbital motion of a test particle orbiting an isolated central body. Here, it is shown that, if it were real, its expected magnitude for the inner planets of the Solar System would be at the same level of the present-day accuracy in constraining any possible deviations from their standard perihelion precessions as inferred from long data records spanning about the last century. The most favorable situation for testing the Verlinde-type precession seems to occur for Mars. Indeed, according to recent versions of the EPM and INPOP planetary ephemerides, non-standard perihelion precessions, of whatsoever physical origin, which are larger than some ≈0.02-0.11 milliarcseconds per century are not admissible, while the putative precession predicted by Liu and Prokopec amounts to 0.09 milliarcseconds per century. Other potentially interesting astronomical and astrophysical scenarios like, e.g., the Earth's LAGEOS II artificial satellite, the double pulsar system PSR J0737-3039A/B and the S-stars orbiting the Supermassive Black Hole in Sgr A * are, instead, not viable because of the excessive smallness of the predicted precessions for them.

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Cosmological perturbations on local systems

Cited by 71 publications

References 35 publications

Weak-field spherically symmetric solutions inf(T)gravity

Weak-field spherically symmetric solutions inf(T)gravity

Solar system tests for realistic f(T) models with non-minimal torsion–matter coupling

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

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