<?xml version="1.0" encoding="UTF-8"?><xml><records><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>47</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">D'Cruz, N. L.</style></author><author><style face="normal" font="default" size="100%">Dickens, R. J.</style></author><author><style face="normal" font="default" size="100%">Hatzidimitriou, D.</style></author><author><style face="normal" font="default" size="100%">Rood, R. T.</style></author><author><style face="normal" font="default" size="100%">O'Connell, R. W.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Calcium abundances of blue horizontal branch stars in ω Centauri.</style></title><short-title><style face="normal" font="default" size="100%">Stellar Ecology: Advances in Stellar Evolution,</style></short-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Globular Clusters: Horizontal-Branch Stars</style></keyword><keyword><style  face="normal" font="default" size="100%">Globular Clusters: Metal Abundances</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">1997</style></year><pub-dates><date><style  face="normal" font="default" size="100%">1997/01/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/1997seas.conf..100D</style></url></web-urls></urls><pages><style face="normal" font="default" size="100%">100 - 104</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">Spectra of 480 blue horizontal branch (BHB) stars in ω Centauri have been obtained using the multiobject fiber spectroscopic facility, Autofib, at the 3.9 m AAT. Preliminary analysis in the temperature range 7500K - 8200K indicates that a large fraction of BHB stars are at lower metallicities compared to the RR Lyrae stars and the giants. This could possibly be used to elucidate how mass loss efficiency varies with metallicity. The data can also be used together with simulated HBs to derive the variation of HB luminosity with metallicity.</style></abstract></record></records></xml>