We report the results of more than seven years of monitoring of PSR J0537 - 6910 , the 16 ms pulsar in the Large Magellanic Cloud , using data acquired with the Rossi X-ray Timing Explorer . During this campaign the pulsar experienced 23 sudden increases in frequency ( “ glitches ” – 21 with increases of at least eight \mu Hz ) amounting to a total gain of over six parts per million of rotation frequency superposed on its gradual spindown of \dot { \nu } = -2 \times 10 ^ { -10 } Hz s ^ { -1 } . The time interval from one glitch to the next obeys a strong linear correlation to the amplitude of the first glitch , with a mean slope of about 400 days per part per million ( 6.5 days per \mu Hz ) , such that these intervals can be predicted to within a few days , an accuracy which has never before been seen in any other pulsar . There appears to be an upper limit of \sim 40 \mu Hz for the size of glitches in all pulsars , with the 1999 April glitch of PSR J0537 - 6910 as the largest so far . The change of its spindown across the glitches , \Delta \dot { \nu } , appears to have the same hard lower limit of - 1.5 \times 10 ^ { -13 } Hz s ^ { -1 } , as , again , that observed in all other pulsars . The spindown continues to increase in the long term , \ddot { \nu } = -10 ^ { -21 } Hz s ^ { -2 } , and thus the timing age of PSR J0537 - 6910 ( -0.5 \nu { \dot { \nu } } ^ { -1 } ) continues to decrease at a rate of nearly one year every year , consistent with movement of its magnetic moment away from its rotational axis by one radian every 10,000 years , or about one meter per year . PSR J0537 - 6910 was likely to have been born as a nearly-aligned rotator spinning at 75–80 Hz , with a | \dot { \nu } | considerably smaller than its current value of 2 \times 10 ^ { -10 } Hz s ^ { -1 } . Its pulse profile consists of a single pulse which is found to be flat at its peak for at least 0.02 cycles . Glitch activity may grow exponentially with a timescale of 170 years \nu \dot { \nu } { ( ( \nu \dot { \nu } ) _ { Crab } } ) ^ { -1 } in all young pulsars .