The Effect of Vertical Datum Inconsistencies on the Determination of Gravity Related Quantities.

Author(s):  
P. Laskowski
Keyword(s):  
2019 ◽  
Vol 63 (01) ◽  
pp. 13-26
Author(s):  
Oskar Sterle ◽  
Božo Koler
Keyword(s):  

2018 ◽  
Vol 36 (1) ◽  
pp. 81
Author(s):  
Éder Teixeira Marques ◽  
William Rodrigo Dal Poz ◽  
Gabriel Do Nascimento Guimarães

ABSTRACT. A vertical reference system is characterized by a vertical datum and a set of scientific altitudes. In the case of orthometric altitudes, the geoid is used as a reference surface, equipotential surface of the gravity field of the Earth that better fits, in the sense of the Least Square Method, to the mean sea level. This study aimed to determine the geoid by applying two processes for calculation of residual ondulation, the integration and the Fast Fourier Transform. These techniques were applied to the values of the residual anomalies obtained from different methods of gravimetric reduction, the Helmert’s Second Method of Condensation, Bouguer and Rudzki. Two test areas were used. For area 1, the best gravimetric geoid was obtained by applying 1D planar FFT with the Helmert’s SecondMethod of Condensation. For area 2, the best gravimetric geoid was obtained through the application of integration and the Rudzki’s reduction. It can be concluded that the physical characteristics of both areas are relevant in the determination of the geoid and that additional procedures must be applied to improve the geoid determination, mainly, in area 2 whose physical characteristics are more heterogeneous than in area 1.Keywords: Geoid, GeoFis 1.0, Gravimetric Reduction, FFT, Stokes Integral. RESUMO. Um sistema vertical de referência é caracterizado por um datum vertical e pelo conjunto de altitudes científicas. No caso das altitudes científicas adotadas serem as ortométricas utiliza-se como superfície de referência o geoide, superfície equipotencial do campo da gravidade da Terra que melhor se ajusta, no sentido do método dos mínimos quadrados, ao nível médio do mar. O objetivo desse trabalho foi determinar o geoide aplicando dois processos de cálculo da ondulação residual, a integração e a Transformada Rápida de Fourier. Essas técnicas foram empregadas aos valores de anomalias residuais obtidas a partir de diferentes métodos de redução gravimétrica, Segundo Método de Condensação de Helmert, Bouguer e Rudzki. Foram utilizadas duas áreas de teste. Verificou-se que para a área 1 o melhor geoide gravimétrico foi obtido pela aplicação da FFT planar 1D juntamente com o Segundo Método de Condensação de Helmert. Para a área 2 o melhor geoide gravimétrico foi obtido pela aplicação da integração e da redução de Rudzki. Conclui-se que as características físicas das duas áreas são relevantes na determinação do geoide e que procedimentos complementares devem ser aplicados para melhorar a determinação do geoide, principalmente, na área 2 cujas características físicas são mais heterogêneas do que da área 1. Palavras-chave: Geoide, GeoFis 1.0, Redução gravimétrica, FFT, Integral de Stokes.


1966 ◽  
Vol 25 ◽  
pp. 93-97
Author(s):  
Richard Woolley

It is now possible to determine proper motions of high-velocity objects in such a way as to obtain with some accuracy the velocity vector relevant to the Sun. If a potential field of the Galaxy is assumed, one can compute an actual orbit. A determination of the velocity of the globular clusterωCentauri has recently been completed at Greenwich, and it is found that the orbit is strongly retrograde in the Galaxy. Similar calculations may be made, though with less certainty, in the case of RR Lyrae variable stars.


1999 ◽  
Vol 190 ◽  
pp. 549-554
Author(s):  
Nino Panagia

Using the new reductions of the IUE light curves by Sonneborn et al. (1997) and an extensive set of HST images of SN 1987A we have repeated and improved Panagia et al. (1991) analysis to obtain a better determination of the distance to the supernova. In this way we have derived an absolute size of the ringRabs= (6.23 ± 0.08) x 1017cm and an angular sizeR″ = 808 ± 17 mas, which give a distance to the supernovad(SN1987A) = 51.4 ± 1.2 kpc and a distance modulusm–M(SN1987A) = 18.55 ± 0.05. Allowing for a displacement of SN 1987A position relative to the LMC center, the distance to the barycenter of the Large Magellanic Cloud is also estimated to bed(LMC) = 52.0±1.3 kpc, which corresponds to a distance modulus ofm–M(LMC) = 18.58±0.05.


1961 ◽  
Vol 13 ◽  
pp. 29-41
Author(s):  
Wm. Markowitz
Keyword(s):  

A symposium on the future of the International Latitude Service (I. L. S.) is to be held in Helsinki in July 1960. My report for the symposium consists of two parts. Part I, denoded (Mk I) was published [1] earlier in 1960 under the title “Latitude and Longitude, and the Secular Motion of the Pole”. Part II is the present paper, denoded (Mk II).


1972 ◽  
Vol 1 ◽  
pp. 27-38
Author(s):  
J. Hers

In South Africa the modern outlook towards time may be said to have started in 1948. Both the two major observatories, The Royal Observatory in Cape Town and the Union Observatory (now known as the Republic Observatory) in Johannesburg had, of course, been involved in the astronomical determination of time almost from their inception, and the Johannesburg Observatory has been responsible for the official time of South Africa since 1908. However the pendulum clocks then in use could not be relied on to provide an accuracy better than about 1/10 second, which was of the same order as that of the astronomical observations. It is doubtful if much use was made of even this limited accuracy outside the two observatories, and although there may – occasionally have been a demand for more accurate time, it was certainly not voiced.


2000 ◽  
Vol 179 ◽  
pp. 205-208
Author(s):  
Pavel Ambrož ◽  
Alfred Schroll

AbstractPrecise measurements of heliographic position of solar filaments were used for determination of the proper motion of solar filaments on the time-scale of days. The filaments have a tendency to make a shaking or waving of the external structure and to make a general movement of whole filament body, coinciding with the transport of the magnetic flux in the photosphere. The velocity scatter of individual measured points is about one order higher than the accuracy of measurements.


1975 ◽  
Vol 26 ◽  
pp. 341-380 ◽  
Author(s):  
R. J. Anderle ◽  
M. C. Tanenbaum

AbstractObservations of artificial earth satellites provide a means of establishing an.origin, orientation, scale and control points for a coordinate system. Neither existing data nor future data are likely to provide significant information on the .001 angle between the axis of angular momentum and axis of rotation. Existing data have provided data to about .01 accuracy on the pole position and to possibly a meter on the origin of the system and for control points. The longitude origin is essentially arbitrary. While these accuracies permit acquisition of useful data on tides and polar motion through dynamio analyses, they are inadequate for determination of crustal motion or significant improvement in polar motion. The limitations arise from gravity, drag and radiation forces on the satellites as well as from instrument errors. Improvements in laser equipment and the launch of the dense LAGEOS satellite in an orbit high enough to suppress significant gravity and drag errors will permit determination of crustal motion and more accurate, higher frequency, polar motion. However, the reference frame for the results is likely to be an average reference frame defined by the observing stations, resulting in significant corrections to be determined for effects of changes in station configuration and data losses.


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