(Summary) The functional conditions referring the anomalous potential have been worked out by the integral formula of Green. The value of the functionals over the continental areas has been calculated by the measured values of the gravity anomaly and the components of deflection of the vertical or of the geopotential number and for ocean areas by the measured values of the gravity disturbance or of the boundary values of the potential. The functional problem has been reduced to the restoration of the
finite-dimensional and unique geopotential which satisties the functional cxonditions best /in least-squares sense/. The discretisation of the functional could be carried out by means of a complete system of expansion unorthogonal functions. By the preliminary orthonormalization of this system the problem has been reduced to a system of linear equations, referring the coeficients of Fourier in the expansion of the potential. We propose four spherical solutions of the altimetry-gravimetry boundary problem by a discrete description and two in a closed form by a generalisation of the function of Stokes and Neumann /Hotine kernel/.
The dominant forces determining the motion of interplanetary particulates are gravitation, solar radiation pressure and Lorentz force. The latter two becoming significant for micron- and submicron- sized particles. In situ measurements by spaceprobes, microcrater distributions and remote observations both in the IR and visible wavelength range have established the mass frequency and spatial distribution of dust particles in interplanetary space. Consequences of the Poynting-Robertson effect and mutual collisions on these distributions and the contributions of various sources (interstellar dust, asteroids and comets) are discussed. It is shown that the contribution from a distributed source of large particles in the inner solar system is most important. Collisions between these meteor sized particles (m > 10^-5 g) produce large amounts of zodiacal light particles (10^-5 g to 10^-10 g) and
β-meteoroids (m < 10^-10 g) which leave the solar system on hyperbolic orbits. At the present time the Poynting-Robertson effect transports into the inner solar system less than 10% of the zodiacal light particles which are produced by collisions from bigger particles.
The paper describes the instrument´s design, technique and some results of measurements of the main solar wind kinetic parameters, made aboard the Prognoz 8 satellite by a Soviet-Czechoslovak energy spectrometer. The aim of this experiment was to test the technique of shock wave detection through readings of the plasma instrument and to measure plasma parameters with high time resolution (up to 1.3 s).
Aus den photographischen und visuellen Kometenhelligkeiten werden die photometrischen Parameter m0 und n berechnet. Es zeigt sichm dass die absolute Helligkeit der durchschnittlichen Grösse m0 der meisten Kometen gleich sind. Der Exponent n ist aber verhältnissmassig klein, nesonders für die visuellen Beobachtungen. Der Farbenindex änderte sich mit wachsendem Abstand des Kometen von der Sonne.
This paper presents measurements of the polarization of light in the tails of the comets Arend-Roland and Mrkos, made in the total photographic light. Results given in Tables II and V indicate that the tail of the Arend-Roland comet contained a substantial dust component, while the polarization in the tail of the Mrkos comet can be explained predominantly by pure molecular emission.
We report on simultaneous profiles measurements obtained in the La, Lp, MglI and Call lines in a sunspot umbra and penumbra, performed with the L. P. S. P. instrument on OSO 8. Although the statistic does not allow for a full time coverage in all lines, we are able to analyze CalI H and K shifts and intensity variations, along
with calibrated average profiles in other lines. Results are compared with other observations and predictions of the acoustic model.