Proper motions, absolute magnitudes and spatial distribution of Zirconium stars

Abstract

The computational algorithm to determine the the proper motions of Zirconium stars on the basis of catalogues "Carte du Ciel" and on the recent photographic observations carried out with the 70cm Abastumani meniscus telescope is presented. It allowed to determine the proper IntroductionFor more detailed study of red giants it is needed to have the space distribution parameters for which a precise scale distances should be determined. Unfortunately, the statistical parallaxes are almost the only way to determine the distance scale of Zirconium stars (ZS).Here were investigated Mira Ceti long-period variable Zirconium stars (MCLPZS) and low-amplitude variables and stationary Zirconium stars (LASZS). All previous determinations of the absolute magnitudes of ZS are given in More recent investigations of ZS were given by Yorka and Wing (1979), Catchpole (1989), Feast (1989) , Catchpole and Feast( 1985) , and others. Yorka and Wing (1979) conclude that MCLPZS at maximum are brighter than non-Mira ZS, but are not as bright as Mv = -3.0. The surface distribution of all known ZS stars indicates that most of them belong to the older Population I. 219We suppose that the differences caused by the following factors: