By B. Morando (auth.), Bruno Morando (eds.)
This e-book gathers the court cases of a symposium on Dynamics of satellites which happened in Prague in may well 1969 through the 12th COSPAR assembly. This symposium was once backed via the overseas Astronomical Union, the overseas organization of Geodesy, the foreign Union of Theoretical and utilized Mechanics and COSPAR (Committee on house Research). The organizing committee was once composed of Dr. KOVALEVSKY chair guy, Dr. Yu. V. BATRAKOV representing IAU, Dr. A. H. cook dinner for lAG, Dr. D. KING-HELE for COSPAR, Prof. M. Roy for IUTAM and Dr. ROSENBERG. I desire to make the most of the chance to thank, on behalf of the entire individuals, the organizing committee contributors, Prof. BUCHAR, Dr. RAJSK:I and Dr. SEHNAL, for the kindness and potency in their welcome. The interpreters who translated with virtuosity in the course of the entire symposium additionally deserve our gratitude. i'm thankful additionally for the care and ability with which Springer-Verlag has revealed this volume.
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Additional info for Dynamics of Satellites (1969): Proceedings of a Symposium held in Prague, May 20–24, 1969
The accuracy of the elements can be considerably increased when the observations occur to be distributed on two short arcs (u 1 , u 2 and U 3 , u 4 ) removed from each other at an arbitrary angle L1 W. In this case the expressions for q(i), q(Q) , q(M + co), q(a x} , q(ay) + q(n) q(M q (a y) w) 1 (l LJ n 2 Rin 2'i cos U) 3 (l T2 2) + ~ (~ I- (1,2 I- 15 LJ u ~~~_SiIl2 i ~ ~2 cos2i (1 - (lLJu 2(y2-+- 45LJu4) . + cos U) + ~ LJ u 4) U 2) 6 ( y + LJ -3(1 (l;j u 2(y2 i)] Sin 2 (} A Z q(Q) q (ax) A,z 6(1 - cos U) (l sin 2 i LJ u 2 U 2 ) (1 - cos U) 6 ( Y + LJ -3- A, Z, Q 6 (1 + cos U) (3 LJ u 2 q (i) Table 1.
3. Results on the Gravitational Field of the Moon The results which have been obtained for the coefficients in the lunar gravitational potential to date are considerably affected both by the number of coefficients which are included in the approximations and by the extent of global coverage of the moon inherent in the data. used for the analyses. Various authors have used different degrees of approximations to the infinite series expansion of the potential and no two solutions published so far have numerical values for the same set of coefficients.
200 240 mm 280 Fig. 2. L05 Doppler residuals. high-frequency oscillations in the residuals still exist, particularly near pericenter for high eccentricity orbits and generally throughout the orbit for low-altitude, nearly circular orbits. The residual plots shown in Figs. 1 and 2 illustrate the reduction in the magnitude of residuals between an intermediate 9th-degree field and the 13th-degree field of Table 3, and the characteristics of the residuals remaining after the 13th-degree field solution, for data from Lunar Orbiters III and V.
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