Hostname: page-component-586b7cd67f-l7hp2 Total loading time: 0 Render date: 2024-11-26T06:51:39.450Z Has data issue: false hasContentIssue false
  • English
  • Français

Intensive X-ray Monitoring of the 16ms Crab-like Pulsar PSR J0537 – 6910

Published online by Cambridge University Press:  12 April 2016

F. E. Marshall ,
E. V. Gotthelf ,
J. Middleditch ,
Q. D. Wang  and
W. Zhang
F. E. Marshall
Affiliation:
Lab. for High Energy Astrophysics, NASA/GSFC, Greenbelt, MB 20771
E. V. Gotthelf
Affiliation:
Columbia Astrophysics Lab., 550 West 120th St, New York, NY 10027
J. Middleditch
Affiliation:
Los Alamos National Lab., MS B256, CIC-3, Los Alamos, NM 87545
Q. D. Wang
Affiliation:
Dept. of Astronomy, Univ. of Massachusetts, Amherst, MA 01003
W. Zhang
Affiliation:
Lab. for High Energy Astrophysics, NASA/GSFC, Greenbelt, MD 20771

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The recently discovered pulsar PSR J0537-6910 is the most rapidly rotating young pulsar known. This latest example of a Crab-like pulsar, located in the supernova remnant N157B in the Large Magellanic Cloud, is rotating twice as fast as the Crab pulsar. With a characteristic age of 5000 years, it is also the oldest known example of a Crab-like pulsar and was likely rotating close to the maximum rate for a neutron star when it was born. Here we report preliminary results from an intensive monitoring campaign of X-ray observations acquired with the Rossi X-ray Timing Explorer that began in January 1999. These observation have revealed a large glitch event in the pulse timing during the first six month of our campaign, consistent with those suggested by sparse observations dating back to 1993. The current evolution of the rotation rate of PSR J0537-6910 provides a unique probe of the internal structure of neutron stars and constraints on possible pulsar emission mechanisms.

Type
Part 5. High-Energy Observations
Information
International Astronomical Union Colloquium , Volume 177: Pulsar Astronomy - 2000 and Beyond , 2000 , pp. 335 - 340
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Allen, M.P. & Horvath, J.E. 1997, MNRAS, 287, 615.Google Scholar
Bradt, H.V., Rothschild, R.E. & Swank, J.H. 1993, A&AS, 97, 355.Google Scholar
Link, B. & Epstein, R.J. 1997, ApJ, 478, L91.Google Scholar
Link, B. et al. 1998, ApJ, 508, 838.Google Scholar
Lyne, A.G. 1995, in Lives of Neutron Stars, p. 167.Google Scholar
Lyne, A.G. et al. 1996, MNRAS, 281, L14.Google Scholar
Marshall, F.E. et al. 1998 ApJ, 499, L179.Google Scholar
McKenna, J. & Lyne, A.G. 1990, Nature, 343, 349.Google Scholar
Rots, A.H. et al. 1998, ApJ, 501, 749.Google Scholar
Shemar, S.L. & Lyne, A.G. 1996, MNRAS, 282, 677.Google Scholar
Wang, Q.D. & Gotthelf, E.V. 1998a, ApJ, 494, 623.Google Scholar
Wang, Q.D. & Gotthelf, E.V. 1998b, ApJ, 509, L109.Google Scholar