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Title:
A Giant Glitch in the Energetic 69 Millisecond X-Ray Pulsar AXS J161730-505505
Authors:
Torii, Ken'ichi; Gotthelf, E. V.; Vasisht, G.; Dotani, T.; Kinugasa, K.
Affiliation:
AA(Space Utilization Research Program, Tsukuba Space Center, National Space Develop Agency of Japan, 2-1-1, Sengen, Tsukuba, Ibaraki, 305-8505, Japan; ), AB(Columbia Astrophysics Laboratory, 550 West 120th Street, New York, NY 10027; ), AC(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109; ), AD(Institute of Space and Astronautical Science, 3-1-1, Yoshinodai, Sagamihara, Kanagawa, 229-8510, Japan; ), AE(Gunma Astronomical Observatory, 6860-86, Nakayama, Takayama, Agatsuma, Gunma, 377-0702, Japan; )
Publication:
The Astrophysical Journal, Volume 534, Issue 1, pp. L71-L74. (ApJL Homepage)
Publication Date:
05/2000
Origin:
UCP
ApJ Keywords:
STARS: PULSARS: GENERAL, STARS: PULSARS: INDIVIDUAL: ALPHANUMERIC: AXS J161730-505505, STARS: PULSARS: INDIVIDUAL: ALPHANUMERIC: PSR J1617-5055, STARS: NEUTRON, ISM: SUPERNOVA REMNANTS, X-RAYS: GENERAL
DOI:
10.1086/312656
Bibliographic Code:
2000ApJ...534L..71T

Abstract

We present new results on the recently discovered 69 ms X-ray pulsar AXS J161730-505505, the sixth youngest example of a rotation-powered pulsar. We have undertaken a comprehensive X-ray-observing campaign of AXS J161730-505505 with the ASCA, BeppoSAX, and RXTE observatories and follow its long-term spin-down history between 1989 and 1999 using these observations and archival Ginga and ASCA data sets. The spin-down is not simply described by a linear function as originally thought, but instead we find evidence of a giant glitch (ΔP/P>~10-6) between 1993 August and 1997 September, perhaps the largest yet observed from a young pulsar. The glitch is well described by steps in P and P accompanied by a persistent P similar to those seen in the Vela pulsar. The pulse profile of AXS J161730-505505 presents a single asymmetric peak that is maintained over all observation epochs. The energy spectrum is also steady over time, characterized by a highly absorbed power law with a photon index Γ=1.4+/-0.2, consistent with that found for other young rotation powered pulsars.
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