000002873 001__ 2873
000002873 005__ 20160701171712.0
000002873 0247_ $$2DOI$$a10.1017/S1743921309991724
000002873 037__ $$aASTROimport-1030
000002873 100__ $$aMartayan, C.
000002873 245__ $$aEvolution and appearance of Be stars in SMC clusters
000002873 260__ $$c2010
000002873 520__ $$aStar clusters are privileged laboratories for studying the evolution of massive stars (OB stars). One particularly interesting question concerns the phases during which the classical Be stars occur, which—unlike HAe/Be stars—are not pre-main-sequence objects, nor supergiants. Rather, they are extremely rapidly rotating B-type stars with a circumstellar decretion disk formed by episodic ejections of matter from the central star. To study the impact of mass, metallicity, and age on the Be phase, we observed Small Magellanic Cloud (SMC) open clusters with two different techniques: (i) with the ESO-WFI in slitless mode, which allowed us to find the brighter Be and other emission-line stars in 84 SMC open clusters, and (ii) with the VLT-FLAMES multifiber spectrograph to determine accurately the evolutionary phases of Be stars in the Be-star-rich SMC open cluster NGC 330. Based on a comparison to the Milky Way, a model of Be stellar evolution, appearance as a function of metallicity and mass, and spectral type is developed, involving the fractional critical rotation rate as a key parameter. 
000002873 700__ $$a Baade, D.
000002873 700__ $$a Frémat, Y.
000002873 700__ $$a Zorec, J.
000002873 773__ $$c470-473$$pStar Clusters: Basic Galactic Building Blocks Throughout Time and Space$$v266$$y2010
000002873 85642 $$ahttp://esoads.eso.org/abs/2010IAUS..266..470M
000002873 905__ $$apublished in
000002873 980__ $$aNONREF