Predicting The Glitches In PSR J0537-6910

Details Predicting The Glitches In PSR J0537-6910 Predicting The Glitches In PSR J0537-6910

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.0401m&link_type=abstract

American Astronomical Society Meeting 208, #4.01; Bulletin of the American Astronomical Society, Vol. 38, p.81

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Scientific paper

We report the results of more than 7 years of monitoring of PSR J0537-6910, the 16 ms pulsar in the LMC, using data acquired with the PCA of the Rossi X-Ray Timing Explorer. During this campaign the pulsar experienced some 20 glitches of at least 8 uHz in amplitude, amounting to a total gain of over 6 ppm in its 62 Hz spin frequency, superposed on its spindown of -0.2 nHz/s. The time interval from one glitch to the next obeys a strong linear correlation to the amplitude of the 1st glitch, with a mean slope of about 400 days/ppm, such that these intervals can be predicted to an accuracy of a few days. The ability to predict the time of the next glitch to this accuracy has never before been seen in any other pulsar. There appears to be an absolute upper limit of 40 uHz for the size of glitches in all pulsars. The change in spindown across a glitch also appears to have a hard limit of -0.15 pHz/s, again in all other pulsars as well as J0537. The longterm trend in the spindown of -1.e-21 Hz/s/s, the low magnitude of the spindown (wrt the Crab), and the singly-peaked pulse profile suggest that J0537 was born as a nearly aligned rotator and that its magnetic pole may be migrating away from the rotation axis at a rate of about a radian in 10,000 years. The initial spin frequency of J0537 4,000 years ago was likely between 75 and 80 Hz, and its initial spindown rate was considerably lower than the present day value of -0.2 nHz/s.

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