COMMISSION 27 OF THE I. A. U. INFORMATION BULLETIN ON VARIABLE STARS Number 1122 Konkoly Observatory Budapest 1976 April 5 CHANGES IN THE PERIOD OF XZ ANDROMEDAE One of the hypotheses explains changes in the period of XZ And by the motion of apsidal line (cf. Todoran, 1967). Unfortunately, there are some difficulties in the determination of accurate times of secondary minima which are very shallow. Only photoelectrical observations are useful for this purpose. Table 1 contains the times of secondary minima obtained from photoelectrical observations published by Blitzstein (1954) and Reinhardt (1967). The last minimum was observed by the writer with the 50 cm Cassegrain-telescope of the Astronomical Observatory in Cracow. The values of O-C and E was computed from the linear elements: Primary minimum = 242 3977.1915 + 1.357278d E Secondary minimum = 242 3977.8701 Table 1 Secondary minima of XZ And J.D. hel. E O-C Observer 243 3231.7415 + 6818 -0.0500 Blitzstein 243 9020.5507 +11083 -0.0315 Reinhardt 244 2742.2476 +13825 +0.0092 Kreiner The O-C diagram of XZ And is given in Fig. 1. The diagram is constructed on the basis of Todoran's paper (1967) and completed [FIGURE 1] with visual observations up to January 1976. The crosses on the O-C curve represent the secondary minima. The position of secondary minima on the O-C diagram excludes the explanation of the observed changes in the period by apsidal motion. J. M. KREINER Astronomical Observatory of the Jagiellonian University, Cracow, Poland. References: Blitzstein, W., 1954, A.J. 59, 251 [BIBCODE 1954AJ.....59..251B ] Reinhardt, M., 1967, A.N. 290, 19 [BIBCODE 1967AN....290...19R ] Todoran, I., 1967, B.A.C. 18, 328 [BIBCODE 1967BAICz..18..328T ]