<?xml version="1.0" encoding="UTF-8"?><xml><records><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Gazeas, K. D.</style></author><author><style face="normal" font="default" size="100%">Niarchos, P. G.</style></author><author><style face="normal" font="default" size="100%">Boutsia, K. A.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">SZ Lyn: New pulsational and orbital elements based on old and recent photometric observations</style></title><short-title><style face="normal" font="default" size="100%">Communications in Asteroseismology</style></short-title></titles><dates><year><style  face="normal" font="default" size="100%">2004</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2004/06/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2004CoAst.145...49G</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">145</style></volume><pages><style face="normal" font="default" size="100%">49</style></pages><isbn><style face="normal" font="default" size="100%">1021-2043</style></isbn><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">SZ Lyncis (=HD 67390) is a high amplitude Delta Scuti star, discovered by Hoffmeister in 1949. Van Genderen (1967) noticed that the residuals in the O-C diagrams followed a sinusoidal variation with a period of Porb = 3.091 years. Several years later, Barnes &amp; Moffett (1975) improved this period to Porb = 3.138 years and suggested that the sinusoidal variations in the O-C diagrams, observed by van Genderen (1967), originate from the light travel time effect, since SZ Lyn is a member of a binary system. This hypothesis was confirmed by Bardin &amp; Imbert (1984) with measurements of radial velocities. Soliman et al. (1986) found the pulsation period to be 0.120534896 days and the orbital period 1173.5 days.</style></abstract></record></records></xml>