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In this paper, the expressions of variations of the dynamical ellipticity and the principal moments of inertia due to the
deformations produced by the zonal part of the tidal potential are obtained. Starting from these expressions, we have studied
from equations related to Hamiltonian theory, their effects on the nutation and finally we have evaluated numerically such
influences, with a level of truncation at 0.1 μas. Thus we have shown that some coefficients are quite large with respect
to the usual accuracy of up-to-date observations.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
2.
Marta Folgueira Jean Souchay Hiroshi Kinoshita 《Celestial Mechanics and Dynamical Astronomy》1997,69(4):373-402
In this paper, we calculate the coefficients of the nutation for a rigid Earth model due to the C
3m and S
3m (m ≠ 0) harmonics of the geopotential, starting from the Hamiltonian theory as developped by Kinoshita (1977). We show that
these coefficients are far from being negligible as given the level of truncation of 0.1 μas which is necessary in the reconstruction
of the tables of nutation, and also that their value is very close to that given by Bretagnon et al. (1997).
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
3.
Effects of the Triaxiality on the Rotation of Celestial Bodies: Application to the Earth,Mars and Eros 总被引:1,自引:0,他引:1
In this paper we discuss the influence of the triaxiality of a celestialbody on its free rotation, i.e. in absence of any external gravitationalperturbation. We compare the results obtained through two different analytical formalisms, one established from Andoyer variables by usingHamiltonian theory, the other one from Euler's variables by usingLagrangian equations. We also give a very accurate formulation of thepolar motion (polhody) in the case of a small amplitude of this motion.Then, we carry out a numerical integration of the problem, with aRunge–Kutta–Felberg algorithm, and for the two kinds of methods above, that we apply to three different celestial bodies considered as rigid : the Earth, Mars, and Eros. The reason of this choice is that each of this body corresponds to a more or less triaxial shape.In the case of the Earth and Mars we show the good agreement betweenanalytical and numerical determinations of the polar motion, and theamplitude of the effect related to the triaxial shape of the body, whichis far from being negligible, with some influence on the polhody of theorder of 10 cm for the Earth, and 1 m for Mars. In the case of Eros, weuse recent output data given by the NEAR probe, to determine in detailthe nature of its free rotational motion, characterized by the presence ofimportant oscillations for the Euler angles due to the particularly largetriaxial shape of the asteroid. 相似文献
4.
M. Folgueira CH. Bizouard J. Souchay 《Celestial Mechanics and Dynamical Astronomy》2001,81(3):191-217
We present a comparison of the diurnal and subdiurnal terms of the three last theories of rigid Earth's rotation: SMART97, RDAN97 and REN 2000. For a better interpretation of the observations, we characterize their contribution to the polar motion and we estimate the non-rigid effects, which are at the level of a few microarcseconds. 相似文献
5.
marta Folgueira Jean Souchay Hiroshi Kinoshita 《Celestial Mechanics and Dynamical Astronomy》1998,70(3):147-157
In this paper, we make a study about the influence of the coefficients of the geopotential C4,m and S4,m, (m=1,2,3,4) on the nutation, starting from the Hamiltonian theory as developed by Kinoshita (1977).We obtain ten coefficients
larger than 0.05 μ as for the nutation in longitude and six for the nutation in obliquity. The present results are included
in the reconstruction of the theory of nutation (REN‐2000) at the level of truncation of 0.1 μ as (Souchay et al., 1997).
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
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