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Title: Solar system constraints on planetary Coriolis-type effects induced by rotation of distant masses

Abstract

We phenomenologically put local constraints on the rotation of distant masses by using the planets of the solar system. First, we analytically compute the orbital secular precessions induced on the motion of a test particle about a massive primary by a Coriolis-like force, treated as a small perturbation, in the case of a constant angular velocity vector Ψ directed along a generic direction in space. The semimajor axis a and the eccentricity e of the test particle do not secularly change, contrary to the inclination I, the longitude of the ascending node Ω, the longitude of the pericenter varpi and the mean anomaly M. Then, we compare our prediction for (dot varpi) with the corrections Δdot varpi to the usual perihelion precessions of the inner planets recently estimated by fitting long data sets with different versions of the EPM ephemerides. We obtain as preliminary upper bounds |Ψ{sub z}| ≤ 0.0006−0.013 arcsec cty{sup −1}, |Ψ{sub x}| ≤ 0.1−2.7 arcsec cty{sup −1}, |Ψ{sub y}| ≤ 0.3−2.3 arcsec cty{sup −1}. Interpreted in terms of models of space-time involving cosmic rotation, our results are able to yield constraints on cosmological parameters like the cosmological constant Λ and the Hubble parameter H{sub 0} not toomore » far from their values determined with cosmological observations and, in some cases, several orders of magnitude better than the constraints usually obtained so far from space-time models not involving rotation. In the case of the rotation of the solar system throughout the Galaxy, occurring clockwise about the North Galactic Pole, our results for Ψ{sub z} are in disagreement with the expected value of it at more than 3−σ level. Modeling the Oort cloud as an Einstein-Thirring slowly rotating massive shell inducing Coriolis-type forces inside yields unphysical results for its putative rotation.« less

Authors:
 [1]
  1. Ministero dell'Istruzione, dell'Università e della Ricerca (M.I.U.R.), Fellow of the Royal Astronomical Society (F.R.A.S.), Viale Unità di Italia 68, 70125, Bari (Italy)
Publication Date:
OSTI Identifier:
22272826
Resource Type:
Journal Article
Journal Name:
Journal of Cosmology and Astroparticle Physics
Additional Journal Information:
Journal Volume: 2010; Journal Issue: 08; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 1475-7516
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ANGULAR VELOCITY; ASTROPHYSICS; COMPARATIVE EVALUATIONS; CORRECTIONS; COSMOLOGICAL CONSTANT; GALAXIES; LIMITING VALUES; MASS; PLANETS; PRECESSION; ROTATION; SOLAR SYSTEM; SPACE-TIME; SPACE-TIME MODEL; TEST PARTICLES

Citation Formats

Iorio, Lorenzo. Solar system constraints on planetary Coriolis-type effects induced by rotation of distant masses. United States: N. p., 2010. Web. doi:10.1088/1475-7516/2010/08/030.
Iorio, Lorenzo. Solar system constraints on planetary Coriolis-type effects induced by rotation of distant masses. United States. https://doi.org/10.1088/1475-7516/2010/08/030
Iorio, Lorenzo. 2010. "Solar system constraints on planetary Coriolis-type effects induced by rotation of distant masses". United States. https://doi.org/10.1088/1475-7516/2010/08/030.
@article{osti_22272826,
title = {Solar system constraints on planetary Coriolis-type effects induced by rotation of distant masses},
author = {Iorio, Lorenzo},
abstractNote = {We phenomenologically put local constraints on the rotation of distant masses by using the planets of the solar system. First, we analytically compute the orbital secular precessions induced on the motion of a test particle about a massive primary by a Coriolis-like force, treated as a small perturbation, in the case of a constant angular velocity vector Ψ directed along a generic direction in space. The semimajor axis a and the eccentricity e of the test particle do not secularly change, contrary to the inclination I, the longitude of the ascending node Ω, the longitude of the pericenter varpi and the mean anomaly M. Then, we compare our prediction for (dot varpi) with the corrections Δdot varpi to the usual perihelion precessions of the inner planets recently estimated by fitting long data sets with different versions of the EPM ephemerides. We obtain as preliminary upper bounds |Ψ{sub z}| ≤ 0.0006−0.013 arcsec cty{sup −1}, |Ψ{sub x}| ≤ 0.1−2.7 arcsec cty{sup −1}, |Ψ{sub y}| ≤ 0.3−2.3 arcsec cty{sup −1}. Interpreted in terms of models of space-time involving cosmic rotation, our results are able to yield constraints on cosmological parameters like the cosmological constant Λ and the Hubble parameter H{sub 0} not too far from their values determined with cosmological observations and, in some cases, several orders of magnitude better than the constraints usually obtained so far from space-time models not involving rotation. In the case of the rotation of the solar system throughout the Galaxy, occurring clockwise about the North Galactic Pole, our results for Ψ{sub z} are in disagreement with the expected value of it at more than 3−σ level. Modeling the Oort cloud as an Einstein-Thirring slowly rotating massive shell inducing Coriolis-type forces inside yields unphysical results for its putative rotation.},
doi = {10.1088/1475-7516/2010/08/030},
url = {https://www.osti.gov/biblio/22272826}, journal = {Journal of Cosmology and Astroparticle Physics},
issn = {1475-7516},
number = 08,
volume = 2010,
place = {United States},
year = {Sun Aug 01 00:00:00 EDT 2010},
month = {Sun Aug 01 00:00:00 EDT 2010}
}