<?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%">Antoniou, V.</style></author><author><style face="normal" font="default" size="100%">Zezas, A.</style></author><author><style face="normal" font="default" size="100%">Hatzidimitriou, D.</style></author><author><style face="normal" font="default" size="100%">Kalogera, V.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Small Magellanic Cloud: Star-Formation History and X-Ray Binary Populations</style></title><short-title><style face="normal" font="default" size="100%">9th International Conference of the Hellenic Astronomical Society</style></short-title></titles><dates><year><style  face="normal" font="default" size="100%">2010</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2010/07/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2010ASPC..424..230A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">424</style></volume><pages><style face="normal" font="default" size="100%">230</style></pages><isbn><style face="normal" font="default" size="100%">1050-3390</style></isbn><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">Using Chandra, XMM-Newton and optical photometric catalogs we study the young XRB populations of the SMC. We find that the Be-XRBs are observed in regions with star formation (SF) rate bursts ˜25-60 Myr ago. The similarity of this age with the age of maximum occurrence of the Be phenomenon (˜40 Myr) indicates that the presence of a circumstellar decretion disk plays a significant role in the number of observed XRBs in the 10-100 Myr age range. We also find that regions with strong but more recent SF (e.g. the Wing) are deficient in Be-XRBs. By correlating the number of observed Be-XRBs with the formation rate of their parent populations, we measure a Be-XRB production rate of ˜1 system per 10&lt;SUP&gt;-6&lt;/SUP&gt; M&lt;SUB&gt;sun&lt;/SUB&gt;/yr. Finally, we use the strong localization of the Be-XRB systems in order to set limits on the kicks imparted on the neutron star during the supernova explosion.</style></abstract></record></records></xml>