Discovery of a Glitch in the Accretion Powered Pulsar SXP 1062

Abstract

We present timing analysis of the accretion powered pulsar SXP 1062, based on the observations of \textit{Swift}, \textit{XMM-Newton} and \textit{Chandra} satellites covering a time span of about 2 years. We obtain a phase coherent timing solution which shows that SXP 1062 has been steadily spinning down with a rate $-4.29(7)\times 10^{-14}$ Hz s${}^{-1}$ leading to a surface magnetic field estimate of about $1.5\times 10^{14}$ G. We also resolve the binary orbital motion of the system from X-ray data which confirms an orbital period of 656(2) days. On MJD 56834.5, a sudden change in pulse frequency occurs with $\Delta \nu =1.28(5)\times 10^{-6}$ Hz, which indicates a glitch event. The fractional size of the glitch is $\Delta \nu /\nu \sim 1.37(6)\times 10^{-3}$ and SXP 1062 continues to spin-down with a steady rate after the glitch. A short X-ray outburst 25 days prior to the glitch does not alter the spin-down of the source; therefore the glitch should be associated with the internal structure of the neutron star. While glitch events are common for isolated pulsars, the glitch of SXP 1062 is the first confirmation of the observability of this type of events among accretion powered pulsars. Furthermore, the value of the fractional change of pulse frequency ensures that we discover the largest glitch reported up to now.

arXiv comment19 pages, 5 figures, accepted for publication in MNRAS

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