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Relativistic Reduction of Astrometric Observations at Points Level of Accuracy

Published online by Cambridge University Press:  19 July 2016

V. A. Brumberg ,
S. A. Klioner  and
S. M. Kopejkin
V. A. Brumberg
Affiliation:
(1)Institute of Applied Astronomy, 197042 Leningrad
S. A. Klioner
Affiliation:
(1)Institute of Applied Astronomy, 197042 Leningrad
S. M. Kopejkin
Affiliation:
(2)Sternberg State Astronomical Institute, 119899 Moscow

Abstract

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The framework of general relativity theory (GRT) is applied to the problem of reduction of high precision astrometric observations of the order of one microarcsecond. The equations of geometric optics for the non-stationary gravitational field of the Solar system have been deduced. Integration of the equations of geometric optics results in the isotropic geodesic line connecting the source of emission (a star, a quasar) and an observer. This permits to calculate the effects of relativistic aberration of light due to monopole and quadrupole components of the gravitational field of the Sun and the planets taking into account their motions and rotation. Transformations between the reference systems are used to calculate the light aberration occurring when passing from the satellite system to the geocentric system and from the geocentric system to the baryecntric system. The baryecntric components of the observed position vector reduced to the flat space-time are corrected, if necessary, for parallax and proper motion of a celestial object using the classical techniques of Euclidean geometry.

Type
Part 3: Concepts, Definitions, Models
Information
Symposium - International Astronomical Union , Volume 141: Inertial Coordinate System on the Sky , 1990 , pp. 229 - 240
Copyright
Copyright © Kluwer 1990 

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