Fourier Analysis of the Light Curves of Eclipsing Variables, XVI
Abstract
The practical procedures for the solutions of the elements of any eclipsing system in the frequencydomain have been described in a previous paper of this series (Kopal and Demircan, 1978, Paper XIV). The fundamental quantities from which we depart in quest of our solution are twogfunctions defining by the momentsA _{2m} (see Equations (2.13) (2.16) in Paper XIV, or Equations (3.2) (3.6) in Paper XV: Demircan, 1978b). If we establish the observational values for these functions, they constitute two independent relations between the unknown parametersa andc _{o}, and can be numerically solved for them with the aid of the general expressions for the respective moments. However, the determinacy of these parameters depends on not only the accuracy of observations but also the employedgfunctions. For better understanding of the geometrical determinacy of the eclipse parametersa andc _{o}, different combinations of the momentsA _{2m} have been worked out asgfunctions. For the index 2m, the values between 0 and 6 were applied. It has been noted that the behaviour of these functions vary but very little with applied different combinations of the moments. A choice of the most convenient moments to obtain a good determinacy for the eclipse elements were discussed. In this connection, (i) themdependence of the moments, and the errors in their observational values have been considered, (ii) different practical procedures for the solution of eclipse elements were introduced, and (iii) different type of moments were tested.
 Publication:

Astrophysics and Space Science
 Pub Date:
 July 1978
 DOI:
 10.1007/BF01879577
 Bibcode:
 1978Ap&SS..56..453D
 Keywords:

 Celestial Mechanics;
 Eclipsing Binary Stars;
 Fourier Analysis;
 Light Curve;
 Stellar Occultation;
 Descriptive Geometry;
 Functions (Mathematics);
 Limb Darkening;
 Phase Shift;
 Stellar Atmospheres;
 Astrophysics