The Newtonian and Relativistic Theory of Orbits and the Emission of Gravitational Waves

Laurentis, Mariafelicia De

doi:10.2174/1874381101004010108

Cited by 2 publications

(1 citation statement)

References 93 publications

(155 reference statements)

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“…In order to linearize the field equations ( 4) at first order in h µν , we have to expand around the flat spacetime metric η µν [32,33,34]. Therefore we have…”

Section: Linearized F (R) Gravitymentioning

confidence: 99%

Effective field theory from modified gravity with massive modes

Capozziello

Paolella

Ricciardi

2014

Int. J. Geom. Methods Mod. Phys.

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Massive gravitational modes in effective field theories can be recovered by extending General Relativity and taking into account generic functions of the curvature invariants, not necessarily linear in the Ricci scalar R. In particular, adopting the minimal extension of f (R) gravity, an effective field theory with massive modes is straightforwardly recovered. This approach allows to evade shortcomings like ghosts and discontinuities if a suitable choice of expansion parameters is performed.

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“…In order to linearize the field equations ( 4) at first order in h µν , we have to expand around the flat spacetime metric η µν [32,33,34]. Therefore we have…”

Section: Linearized F (R) Gravitymentioning

confidence: 99%

Effective field theory from modified gravity with massive modes

Capozziello

Paolella

Ricciardi

2014

Int. J. Geom. Methods Mod. Phys.

Self Cite

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Analysis of the Yukawa gravitational potential in f(R) gravity. I. Semiclassical periastron advance

2018

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The concordance cosmological model has been successfully tested over the last decades. Despite its successes, the fundamental nature of dark matter and dark energy is still unknown. Modifications of the gravitational action have been proposed as an alternative to these dark components. The straightforward modification of gravity is to generalize the action to a function, f (R), of the scalar curvature. Thus one is able to describe the emergence and the evolution of the Large Scale Structure without any additional (unknown) dark component. In the weak field limit of the f (R)-gravity, a modified Newtonian gravitational potential arises. This gravitational potential accounts for an extra force, generally called fifth force, that produces a precession of the orbital motion even in the classic mechanical approach. We have shown that the orbits in the modified potential can be written as Keplerian orbits under some conditions on the strength and scale length of this extra force. Nevertheless, we have also shown that this extra term gives rise to the precession of the orbit. Thus, comparing our prediction with the measurements of the precession of some planetary motions, we have found that the strength of the fifth force must be in the range [2.70 − 6.70] × 10 −9 with the characteristic scale length to fix to the fiducial values of ∼ 5000 AU.

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The Newtonian and Relativistic Theory of Orbits and the Emission of Gravitational Waves

Cited by 2 publications

References 93 publications

Effective field theory from modified gravity with massive modes

Effective field theory from modified gravity with massive modes

Analysis of the Yukawa gravitational potential in f(R) gravity. I. Semiclassical periastron advance

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