Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 716, Issue 2, Pages L140-L145Publisher
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/716/2/L140
Keywords
Magellanic Clouds; pulsars: general; stars: early-type; stars: emission-line, Be; stars: formation; X-rays: binaries
Categories
Funding
- NASA LTSA [NAG5-13056, G02-3117X, NNX08AB68G, NNG06GE68G, NNX10AH47G]
- [206469]
- NASA [NNX10AH47G, 133084, NNX08AB68G, 103461] Funding Source: Federal RePORTER
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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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