Force function of two general spheroids

¶rt;um ua u ¶rt; u m, a u an¶rt;u nm m ¶rt;mam uu u¶rt;a ma, m ¶rt; uu u ¶rt; u nmua numu ¶rt;m a u ¶rt;mam m. mau ¶rt;u uu m: m nm u m; a, n¶rt;u au umu u unu¶rt; uuu; amu m u a; amua ¶rt;uam ma a ¶rt; u m um ¶rt;m ma. u ¶rt;a ¶rt; u¶rt;, nuu ¶rt; a, ¶rt;a ¶rt;a ¶rt;o 4- n¶rt;a um.     

Tidal potential due to a non-spherical lunar body

Summary The tidal potential is derived at a point on the Earth's surface for the case when the perturbing gravitational field is not spherically symmetrical.     

The derivatives of the lunar disturbing potential harmonics with respect to euler's angles

Summary The derivatives of the harmonicsP _n ^(k) (sin _O)cos kT_O andP _n ^(k) (sin _O)sin kT_O, occurring in the development of the lunar disturbing potential, are derived upto n=4 and for k== 0, 1, ..., n. The equatorial co-ordinates _OT_O are referred to the Moon's mass centre; the procedure for the solar disturbing potential is formally identical.     

РЕЗУЛЬТАТЫ АНАЛИЗА МЕТОДАМИ ХОЙНИЦКОГО И ВЕНЕДИКОВА ДОЛГОВРЕМЕННЫХ НАБЛЮДЕНИЙ НА ЧЕЩСКНХ ПРИЛИВНЫХ СТАНЦИЯХ

Zusammenfassung Mit Benutzung der langfristigen Gezeitenbeobachtungsreihen mit Hilfe der Klinometer und des Gravimeters auf den tschechoslowakischen Gezeitenstationen werden die Methoden der Analyse von Chojnicki und Venedikov verglichen. Die in Tab. 1–5 zusammengefassten Ergebnisse zeigen beide benutzten Methoden als gleichwertig. Zum Hauptvorteil der Methode von Chojnicki gehört die Möglichkeit der Berechnung von Gezeitenparametern auch für langperiodische Wellen (Tab. 2, 4 und 5).

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3.3 (, 1975).     

Tidal evolution and hydrostatic equilibrium of phobos

Summary A dynamical model of Phobos has been set up: its boundary surface is defined by the 2nd degree Stokes zonal and sectorial parameters, the mass and angular velocity of rotation of the body (assumed homogeneous), plus the constant part of the tidal potential due to Mars which is relatively very large. The tidal evolution has been outlined, based on the condition that, at a certain epoch, the sum of the tidal and centrifugal forces on the surface of Phobos should be equal to the gravitation of opposite sign. The problem of hydrostatic equilibrium of Phobos is discussed.

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ma ¶rt;uaua ¶rt; a: aa nm n¶rt;a m a u mua mu naamau, a u m au ma uma ¶rt;¶rt;, n nm am nuu nmuaa m aa, m aum aum. aa nuua u, aa nu u, m m n a nuu u m u a nmu a aum u numu. ¶rt;am nau¶rt;mamu au a.

     

К определению элементов орБиты спутника по положению и скорости

Summary Orbital problems of satellite geodesy are based on the assumption that the geocentric orbital elements, giving the geocentric position of the satellite being observed, are known for the moment of observation. The determination of such elements, however, is possible only if the observed topocentric quantities were with sufficient accuracy reduced to geocentric ones. The reduction assumes, however, that the position of the satellite stations with respect to the centre of mass of the Earth is known. This, however, is not known and the determination of the geocentric positions is substantially the main problem of present-day geodesy. In the case of natural celestial bodies, relatively far from the basic body, inaccuracies in correcting for the parallax practically do not influence the solution. But in the case of near artificial Earth satellites these inaccuracies are not negligible. The present paper analyzes from this aspect the case when the orbital elements are calculated from one position (three coordinates) and three velocity components. Relations are derived (14, 15, 19, 22, 32, 38) giving the exactly geocentric elements. The way in which they differ from the well-known relations of classical celestial mechanics (10, 11, 17, 20, 24–26, 36), giving only certain approximate elements (we call them quasi-geocentric) consists in considering parameters defining the position of the origin and direction of the axes of the used reference system in the Earth's body. In the derivation we neglected expressions equal in order to the squares of the coordinates of the centre of the reference ellipsoid with respect to the centre of mass of the Earth and to the squares of the angles between the axis of rotation of the ellipsoid and the mean rotation axis of the Earth's inertia as well between the planes of the initial (Greenwich) astronomic and geodetic meridians.

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Адрес: Politickych vězňů 12, Praha 1-Nové Město.