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The Glitches and Rotational History of the Highly Energetic Young Pulsar PSR J0537–6910

Ferdman, R.D.; Archibald, R.F.; Gourgouliatos, K.N.; Kaspi, V.M.

The Glitches and Rotational History of the Highly Energetic Young Pulsar PSR J0537–6910 Thumbnail


Authors

R.D. Ferdman

R.F. Archibald

K.N. Gourgouliatos

V.M. Kaspi



Abstract

We present a timing and glitch analysis of the young X-ray pulsar PSR J0537−6910, located within the Large Magellanic Cloud, using 13 yr of data from the now-decommissioned Rossi X-ray Timing Explorer. Rotating with a spin period of 16 ms, PSR J0537−6910 is the fastest-spinning and most energetic young pulsar known. It also displays the highest glitch activity of any known pulsar. We have found 42 glitches over the data span, corresponding to a glitch rate of 3.2 yr−1, with an overall glitch activity rate of $8.8\times {10}^{-7}\,{\mathrm{yr}}^{-1}$. The high glitch frequency has allowed us to study the glitch behavior in ways that are inaccessible in other pulsars. We observe a strong linear correlation between spin frequency glitch magnitude and wait time to the following glitch. We also find that the post-glitch spin-down recovery is well described by a single two-component model fit to all glitches for which we have adequate input data. This consists of an exponential amplitude $A=(7.6\pm 1.0)\times {10}^{-14}\,{{\rm{s}}}^{-2}$, decay timescale $\tau ={27}_{-6}^{+7}\,\mathrm{day}$s, and linear slope $m=(4.1\pm 0.4)\times {10}^{-16}\,{{\rm{s}}}^{-2}\,{\mathrm{day}}^{-1}$. The latter slope corresponds to a second frequency derivative $\ddot{\nu }=(4.7\pm 0.5)\times {10}^{-22}\,{{\rm{s}}}^{-3}$, from which we find an implied braking index $n=7.4\pm 0.8$. We also present a maximum likelihood technique for searching for periods in event-time data, which we used to both confirm previously published values and determine rotation frequencies in later observations. We discuss the implied constraints on glitch models from the observed behavior of this system, which we argue cannot be fully explained in the context of existing theories.

Journal Article Type Article
Acceptance Date Dec 11, 2017
Online Publication Date Jan 15, 2018
Publication Date Jan 15, 2018
Deposit Date Jan 25, 2018
Publicly Available Date Jan 26, 2018
Journal Astrophysical Journal
Print ISSN 0004-637X
Publisher American Astronomical Society
Peer Reviewed Peer Reviewed
Volume 852
Issue 2
Article Number 123
DOI https://doi.org/10.3847/1538-4357/aaa198
Public URL https://durham-repository.worktribe.com/output/1335989

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Copyright Statement
© 2018. The American Astronomical Society.





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