0000000000226453

AUTHOR

R. López Machí

Improved Method for Orbital Elements Differential Correction.

As was pointed out by IAU in 1976, an important problem in fundamental astronomy is the improvement of the vernal equinox and equator positions. To this aim, it is necessary to know the accurate values of minor planets orbital elements. The classical methods of orbital elements differential corrections are based on linking the observations at different epochs considering equal derivatives respect to the initial and osculating elements. In this paper we present an improved method in which the least squares matrix coefficients is calculated from the integration of the Lagrange planetary equations and its derivatives.

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Automated astrographic plates measuring process

The astrographic plates measuring process applied at the Astronomical Observatory of Valencia has been described.

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Figures of equilibrium in close binary systems

The equilibrium configurations of close binary systems are analyzed. The autogravitational, centrifugal and tidal potentials are expanded in Clairaut's coordinates. From the set of the total potential angular terms an integral equations system is derived. The reduction of them to ordinary differential equations and the determination of the boundary conditions allow a formulation of the problem in terms of a single variable.

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Digital Image Processing in the Analysis of Astrometric Plates

AbstractIn this paper, we display an improvement to our process of semi-automatic measuring of astrometric plates, in which the photometric sensor is substituted by a CCD system of image getting and digitalization. The advantages of this method are analyzed taking into account the possibilities of the image analysis in the space and frequency domain.

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Persistence of Asteroids After a Close Encounter

We present here a first approximation to the planar circular restricted 2 + 2 problem. In this four body problem, we consider that the two secondaries do not affect the primaries but they do influence each other. It can be seen as a model for near collision orbits of two asteroids if the primaries are the Sun and Jupiter ([3], [5]). In particular, we analyze the values of the Jacobi constant of the two asteroids before and after the close approach.

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