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Bounds on graviton mass and constraining Yukawa-like gravitational potential from planetary motion in the solar system
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In this study we used the observed perihelion precession of planetary orbits
in the Solar System in order to constrain theory of Yukawa-type gravity, and
to bound mass of graviton. For that purpose we assumed that the precession
angles of the planets in Yukawa-type gravity should be equal to their
observed values, as well as to the corresponding predictions of General
Relativity (GR). Starting from these requests we constrain Yukawa-like
gravitational potential. The obtained results showed that our estimates for
the range of Yukawa interaction ? at the Solar System scales are in good
agreement with recent experimental constrains. Assuming that the estimated
value of the range of ? corresponds to the Compton wavelength of graviton
?1, we then estimate the upper bound for its mass m1. We found that these
estimates were in agreement with our previous results obtained from the
observed stellar orbits around the Galactic Center (GC).
Title: Bounds on graviton mass and constraining Yukawa-like gravitational potential from planetary motion in the solar system
Description:
In this study we used the observed perihelion precession of planetary orbits
in the Solar System in order to constrain theory of Yukawa-type gravity, and
to bound mass of graviton.
For that purpose we assumed that the precession
angles of the planets in Yukawa-type gravity should be equal to their
observed values, as well as to the corresponding predictions of General
Relativity (GR).
Starting from these requests we constrain Yukawa-like
gravitational potential.
The obtained results showed that our estimates for
the range of Yukawa interaction ? at the Solar System scales are in good
agreement with recent experimental constrains.
Assuming that the estimated
value of the range of ? corresponds to the Compton wavelength of graviton
?1, we then estimate the upper bound for its mass m1.
We found that these
estimates were in agreement with our previous results obtained from the
observed stellar orbits around the Galactic Center (GC).
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