Deceleration in the Earth's rotation due to the Sun

Summary The estimate of the tidal long-term decrease in the angular velocity of the Earth's rotation due to the Sun is given as –(0.8±0.3)×10 ^–22 rad s ^–2. It was computed on the basis of the observed total long-term decrease in , of the observed tidal deceleration of the Moon and the observed decrease in the second-degree zonal Stokes geopotential harmonic term. Adopting the estimate given, the product of the Love number and the tidal phase lag angle due to the Sun (in degrees) comes out as 0.53±0.20.

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am a z nuuu u z mu au u, az : –(0,8±0,3) 10 ^–22 a¶rt; ^–2 . ¶rt; ua n a¶rt;a u , n a¶rt;a nuu u ¶rt;z ¶rt;uu u n a¶rt;a u mz az znmuaz naama ma. u num n au, m nu¶rt;u ua a a z u ( za¶rt;a) a z nuua a (0,53±0,20).

     

Roche equipotentials of the pluto-charon system

Summary The positions of the Lagrangian points of the Pluto-Charon system have been determined using the orthogonal system of cofocal ellipses-hyperbolas, the foci being situated at the centre of mass of the bodies. The tidal distortions of Pluto amount to 30 m, those of charon to 122 m. The tidal forces are believed to influence the figures of the bodies significantly.     

Moments of external disturbing forces in the rotational motion of celestial bodies

am ¶rt; mau mu ma uaumau u m a ma, ua aam ¶rt;uu ¶rt;a ma. a ma aamuam u¶rt;; n¶rt;aam u, m uaumau n nua mu nmu ¶rt; ¶rt;mam u mn, u m uma aua umuoa u nu u unu¶rt; uuu. u¶rt;um amo u, ¶rt;a ¶rt;a ¶rt;o 4- n¶rt;a um.     

Variations in the Earth's rotation and crustal deformations

a mmuu ¶rt; ¶rt;au nm u , a auauu ma mu au u. aamuam m¶rt; a, ma u mua mu ¶rt;au u ¶rt;aa u uma a; m a mu ¶rt;auu m ¶rt;muam 10% m ¶rt;au, a u nuuau m .     

Comparison of satellite and terrestrial gravity data

Summary The integral mean values of gravity on the surface W=W ₀ , obtained from satellite observations with the use of harmonic coefficients[3, 7] and from terrestrial gravity measurements[12], are compared. The squares and products of the harmonic coefficients were neglected, with the exception of [J ₂ ⁽⁰⁾ ] ² , which was taken into account. The Potsdam correction and the geocentric constant are being discussed. The paper ties up with[13–15] and the symbols used are the same. The given problem was treated, e.g., in[2, 4, 6, 8–10]; in the present paper the values of gravity are compared directly.     

Determination of the Geopotential Scale Factor from TOPEX/POSEIDON Satellite Altimetry

The geopotential scale factor R _o = GM/W _o (the GM geocentric gravitational constant adopted) and/or geoidal potential Wo have been determined on the basis of the first year's (Oct 92 – Dec 93) ERS-1/TOPEX/POSEIDON altimeter data and of the POCM 4B sea surface topography model: R _o °=(6 363 672.58°±0.05) m, W _o °=(62 636 855.8°±0.05)m ² s ^–2 . The 2°–°3 cm uncertainty in the altimeter calibration limits the actual accuracy of the solution. Monitoring dW _o /dt has been projected.     

The rotation of the earth between 1955.5 and 1976.5

Summary The difference between the rotational time UT1 and atomic time scale AT was analysed in order to find the secular and periodic variations in the rotational velocity of the Earth. It was found that the length of the mean solar day was increasing by 12.8 ms per century in the interval discussed. As a whole, eleven periodic terms were found, the most significant having the periods of 0.5, 1.0, 6.7 and 11.9 y. The correlation between the long period changes in the Earth's rotation and relative sunspot numbers is shown.     

К определению положения искусственного спутника земли в геодезической системе координат

Summary The present theory of the determination of the position of an Earth satellite from simultaneous measurements of the topocentric coordinates at 2 or more geodetic satellite points is not exact. The inaccuracy is caused by the fact that the measured topocentric coordinates of the satellite are defined in a system in which the directions of the axes are not exactly parallel to the directions of the corresponding axes of the geodetic system in which the coordinates of the satellite points are given; this difference in direction is not respected in the solution. The paper gives an exact solution of the problem. The concepts (4) of geodetic topocentric declination and geodetic hour angle of the satellite, i.e. the declination and hour angle in the geodetic reference system, are introduced. With these quantities the problem of determining the position of the satellite is then solved exactly. There always exist superabundant observations so that the method of least squares can be used. The procedure is outlined for the case of conditioned observations (suitable for 2 satellite geodetic points) and for the case of intermediate observations (suitable for >2 satellite geodetic points).