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Pulsars are rotating neutron stars, sweeping the emission regions from themagnetic poles across our line of sight. Isolated neutron stars lose angularmomentum through dipole radiation and (possibly) particle winds, hence theyslow down extremely steadily, making them amongst the most reliable timingsources available. However, it is well known that younger pulsars can sufferglitches, when they suddenly deviate from their stable rotation period. On 2000January 16 (MJD 51559) the rate of pulsation from the Vela pulsar (B0833-45)showed such a fractional period change of {\rm $3.1\times 10^{-6}$}, thelargest recorded for this pulsar. The glitch was detected and reported by theHobart radio telescope. The speedy announcement allowed the X-ray telescope,Chandra, and others, to make Target of Opportunity observations. The dataplaced an upper limit of 40 seconds for the transition time from the originalto the new period. Four relaxation timescales are found, which are believed tobe due to the variable coupling between the crust and the interior fluid. Oneis very short, about 60 seconds; the others have been previously reported andare 0.56, 3.33 and 19.1 days in length.Comment: Accepted in ApJ

High Time Resolution Observations of the January 2000 Glitch in the Vela Pulsar