<?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%">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%">Star Formation History and X-ray Binary Populations: The Case of the Small Magellanic Cloud</style></title><short-title><style face="normal" font="default" size="100%">The Astrophysical Journal</style></short-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Astrophysics - High Energy Astrophysical Phenomena</style></keyword><keyword><style  face="normal" font="default" size="100%">Be</style></keyword><keyword><style  face="normal" font="default" size="100%">Magellanic Clouds</style></keyword><keyword><style  face="normal" font="default" size="100%">pulsars: general</style></keyword><keyword><style  face="normal" font="default" size="100%">stars: early-type</style></keyword><keyword><style  face="normal" font="default" size="100%">stars: emission-line</style></keyword><keyword><style  face="normal" font="default" size="100%">stars: formation</style></keyword><keyword><style  face="normal" font="default" size="100%">X-rays: binaries</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2010</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2010/06/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2010ApJ...716L.140A</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">716</style></volume><pages><style face="normal" font="default" size="100%">L140 - L145</style></pages><isbn><style face="normal" font="default" size="100%">0004-637X</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 X-ray binary (XRB) populations of the Small Magellanic Cloud. We find that the Be/X-ray binaries (Be-XRBs) are observed in regions with star formation 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 star formation (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 3 × 10&lt;SUP&gt;-3&lt;/SUP&gt; M &lt;SUB&gt;sun&lt;/SUB&gt; yr&lt;SUP&gt;-1&lt;/SUP&gt;. 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>