STAR FORMATION HISTORY AND X-RAY BINARY POPULATIONS: THE CASE OF THE SMALL MAGELLANIC CLOUD

被引：81
作者：
Antoniou, V. [1 ,2 ,3 ]
Zezas, A. [1 ,2 ,4 ]
Hatzidimitriou, D. [4 ,5 ]
Kalogera, V. [6 ]
机构：
[1] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
[2] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece
[3] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA
[4] IESL Fdn Res & Technol Hellas, GR-71110 Iraklion, Crete, Greece
[5] Univ Athens, Dept Phys, Sect Astrophys Astron & Mech, GR-15784 Athens, Greece
[6] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA
来源：
ASTROPHYSICAL JOURNAL LETTERS | 2010年 / 716卷 / 02期
关键词：
Magellanic Clouds; pulsars: general; stars: early-type; stars:; emission-line; Be; stars: formation; X-rays: binaries; CATALOG; METALLICITY; VELOCITIES; SMC; CLUSTERS; PULSARS; FIELD;
D O I：
10.1088/2041-8205/716/2/L140
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
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 similar to 25-60 Myr ago. The similarity of this age with the age of maximum occurrence of the Be phenomenon (similar to 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 similar to 1 system per 3 x 10(-3) M(circle dot) yr(-1). 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.
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收藏
页码：L140 / L145
页数：6
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