Geodetic Rotation of the Sun, Major Planets, and the Moon

Details Geodetic Rotation of the Sun, Major Planets, and the Moon Geodetic Rotation of the Sun, Major Planets, and the Moon

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd..16e..57e&link_type=abstract

Nomenclature, Precession and New Models in Fundamental Astronomy, 26th meeting of the IAU, Joint Discussion 16, 22-23 August 200

Astronomy and Astrophysics

Astronomy

Scientific paper

The problem of the geodetic (relativistic) rotation of the Sun, major planets, and the Moon is studied by using DE404/LE404 ephemeris. For every of these bodies the files of the ecliptic components of the vector of the geodetic rotation were formed over time span from AD1000 to AD3000 at intervals of one day. Using the least-squares method and spectral analysis methods the secular and periodic components of the geodetic rotation vector were determined. The mean longitudes of the planets and the Moon adjusted to DE404/LE404 ephemeris were used. For the Earth the component, orthogonal to the plane of the fixed ecliptic J2000.0 was determined: σ[E]^z=19.1988821"-0.00035370"T+...10^-6 dot λ[3](-34.285" cos λ[3] +149.227" sin λ[3]) +..., where λ[3] is the mean longitude of the Earth, T means the time (TDB) measured in thousand Julian years. This result is in a very good agreement with those found analytically. The method was applied to the other bodies of the solar system and following result were obtained: σ[Me]^z=214.905"+0.024"T+...10^-6 dot λ[1](1086.273" cos λ[1] +4882.227" sin λ[1]) +..., σ[M]^z=19.4950402"-0.0000124"T+...+10^-6 dot D(30.212" cos D - 0.001"sin D)+...+ +10^-6 dot λ[3](-34.280" cos λ[3] +149.204" sin λ[3]) +..., Here λ[1] is the mean longitude of Mercury, D=λ-λ[3]+180° , and λ is the mean geocentric longitude of the Moon. The problem of the geodetic rotation of the origin of DE404/LE404 ephemeris is discussed.

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