English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

In this paper we explicitly work out the secular perturbations induced on allthe Keplerian orbital elements of a test body to order O(e^2) in theeccentricity e by the weak-field long-range modifications of the usualNewton-Einstein gravity due to the Dvali-Gabadadze-Porrati (DGP) braneworldmodel. The Gauss perturbative scheme is used. It turns out that the argument ofpericentre and the mean anomaly are affected by secular rates which areindependent of the semimajor axis of the orbit of the test particle. The firstnonvaishing eccentricity-dependent corrections are of order O(e^2). Forcircular orbits the Lue-Starkman (LS) effect on the pericentre is obtained.Some observational consequences are discussed for the Solar System planetarymean longitudes lambda which would undergo a 1.2\cdot 10^-3 arcseconds percentury braneworld secular precession. According to recent data analysis over92 years for the EPM2004 ephemerides, the 1-sigma formal accuracy indetermining the Martian mean longitude amounts to 3\cdot 10^-3 milliarcseconds,while the braneworld effect over the same time span would be 1.159milliarcseconds. The major limiting factor is the 2.6\cdot 10^-3 arcseconds percentury systematic error due to the mismodelling in the Keplerian mean motionof Mars. A suitable linear combination of the mean longitudes of Mars and Venusmay overcome this problem. The formal, 1-sigma obtainable observationalaccuracy would be \sim 7%. The systematic error due to the present-dayuncertainties in the solar quadrupole mass moment, the Keplerian mean motions,the general relativistic Schwarzschild field and the asteroid ring would amountto some tens of percent.Comment: LaTex2e, 23 pages, 5 tables, 1 figure, 37 references. Second-order  corrections in eccentricity explicitly added. Typos corrected. References  update

On the effects of Dvali–Gabadadze–Porrati braneworld gravity on the orbital motion of a test particle