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Chandra observations of black widow pulsars

Published online by Cambridge University Press:  20 March 2013

P. Gentile ,
M. McLaughlin ,
M. Roberts ,
F. Camilo ,
J. Hessels ,
M. Kerr ,
S. Ransom ,
P. Ray  and
I. Stairs
P. Gentile
Affiliation:
Dept. of Physics, West Virginia University, Morgantown, WV 26506, USA
M. McLaughlin
Affiliation:
Dept. of Physics, West Virginia University, Morgantown, WV 26506, USA
M. Roberts
Affiliation:
Eureka Scientic, Inc., Oakland, California 94602, USA
F. Camilo
Affiliation:
Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA
J. Hessels
Affiliation:
ASTRON, Postbus 2, 7990 AA Dwingeloo, The Netherlands
M. Kerr
Affiliation:
W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA
S. Ransom
Affiliation:
NRAO, 520 Edgemont Road, Charlottesville, Virginia 22093, USA
P. Ray
Affiliation:
Space Science Division, Naval Research Laboratory, Washington, DC 20375-5352, USA
I. Stairs
Affiliation:
Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road Vancouver, BC V6T 1Z1Canada
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Abstract

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We describe the first X-ray observations of binary millisecond pulsars PSR J0023+0923, J1810+1744, J2215+5135, and J2256−1024. All are Fermi gamma-ray sources and three are ‘black-widow’ pulsars, with companions of mass < 0.1 M⊙. Data were taken using the Chandra X-Ray Observatory and covered a full binary orbit for each pulsar. PSRs J2215+5135 and J2256−1024, show significant orbital variability and X-ray flux minima coinciding with eclipses seen at radio wavelengths. This is consistent with intrabinary shock emission characteristic of black-widow pulsars. The other two pulsars, PSRs J0023+0923 and J1810+1744, do not demonstrate significant variability, but are fainter than the other two sources. Spectral fits yield power-law indices that range from 1.4 to 2.3 and blackbody temperatures in the hundreds of eV. The spectrum for PSR J2215+5135 shows a significant hard X-ray component (41% of counts are above 2 keV), which is additional evidence for the presence of intrabinary shock emission.

Keywords

pulsars: generalX-rays: binaries
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S291: Neutron Stars and Pulsars: Challenges and Opportunities after 80 years , August 2012 , pp. 389 - 391
Copyright
Copyright © International Astronomical Union 2013

References

Bangale, P., Roberts, M., McLaughlin, M., et al. 2010, Bulletin of the American Astronomical Society, 42, 680Google Scholar
Kolmogorov, A. N. 1933, G. Ist. Attuari, 4, 83Google Scholar
Stappers, B. W., Gaensler, B. M., Kaspi, V. M., van der Klis, M., & Lewin, W. H. G. 2003, Science, 299, 1372Google Scholar