Abstract
On the Geodetic Rotation of the Major Planets, the Moon and the SunThe problem of the geodetic (relativistic) rotation of the major planets, the Moon and the Sun was studied in the paper by Eroshkin and Pashkevich (2007) only for the components of the angular velocity vectors of the geodetic rotation, which are orthogonal to the plane of the fixed ecliptic J2000. This research represents an extension of the previous investigation to all the other components of the angular velocity vector of the geodetic rotation, with respect to the body-centric reference frame from Seidelmann et al. (2005).
Highlights
The principal gravitational interaction between the major planets, the Moon and the Sun in every relativistic ephemeris is modeled by considering these bodies as non-rotating point masses.an ephemeris of the major bodies of the solar system, based on the relativistic equations of the orbital motion, contains data necessary for the calculation of the secular and periodic components of the angular velocity of the geodetic rotation of these bodies
It is easy to see that the values of the secular parts of the geodetic rotation of each planet depend on its distance from the Sun (Table 2)
The secular terms of geodetic rotation of each planet of the Solar system depend on their distance from the Sun, the mass of which is dominant in the solar system
Summary
The principal gravitational interaction between the major planets, the Moon and the Sun in every relativistic ephemeris is modeled by considering these bodies as non-rotating point masses. The behavior of the components of these angular velocity vectors of the geodetic rotation for the major planets, the Moon and the Sun are depicted in Figures 2 – 12. In these Figures represents the geodetic motion of the equator of a body on the fixed ecliptic. Since the mass of the Sun is dominant in the solar system the main part of the angular velocity vector of the geodetic rotation for each major planet and the Moon is a result of the heliocentric orbital motion of these bodies. Its main part (presented in Figure 12) depends on the orbital motions of Jupiter, as the heaviest planet in the solar system, and Mercury, as the nearest planet to the Sun
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