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X-ray Pulsars in the Small Magellanic Cloud

Published online by Cambridge University Press:  12 May 2006

R. H. D. Corbet ,
M. J. Coe ,
J. Galache ,
S. Laycock ,
C. B. Markwardt  and
F. E. Marshall
R. H. D. Corbet
Affiliation:
X-ray Astrophysics Laboratory, Code 662, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA Universities Space Research Association
M. J. Coe
Affiliation:
Department of Astronomy, University of Southampton, Southampton, SO17 1BJ, UK
J. Galache
Affiliation:
Department of Astronomy, University of Southampton, Southampton, SO17 1BJ, UK
S. Laycock
Affiliation:
Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
C. B. Markwardt
Affiliation:
X-ray Astrophysics Laboratory, Code 662, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA University of Maryland
F. E. Marshall
Affiliation:
X-ray Astrophysics Laboratory, Code 662, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA
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Abstract

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The SMC is now known to contain many more transient X-ray pulsars than would be expected based on a simple scaling of the number of such sources in the Galaxy by the relative mass of the SMC. We have been conducting regular monitoring observations of the SMC with the Proportional Counter Array on the Rossi X-ray Timing Explorer since 1997. This has resulted in the discovery of many of these X-ray pulsars and also provided orbital period measurements from detections of regular outbursts. We can now investigate the differences and similarities of the Galactic and SMC X-ray pulsar populations and consider the origin of the huge SMC X-ray pulsar over-abundance.

Keywords

galaxies: Magellanic CloudsX-rays: binariesstars: neutron