Glitches are sudden accelerations of the rotation rate ν of neutron stars, believed to be driven by the neutron superfluid inside the star's crust and core. They present a wide phenomenology and their amplitudes Δν span over six orders of magnitude. The 21 known glitches of the Vela pulsar are amongst the largest observed (typically Δν/ν∼10^-6) and have very similar characteristics. We wish to explore the population of small-amplitude rotational changes in the Vela pulsar and determine the rate of occurrence and sizes of its smallest glitches. We use high cadence observations of the Vela pulsar taken between 1981 and 2005 by the Mount Pleasant Radio Observatory. An automated, systematic search was carried out that investigates whether a significant change of spin frequency ν and/or the spin-down rate \dot{ν} takes place at any given time. Our study reveals numerous events of all possible signatures (i.e. combinations of Δν and Δ \dot{ν} signs), usually small, with |Δν|/ν<10^-9, which contribute to Vela's timing noise. We also find two glitches that have not been reported before, with respective sizes Δν/ν of (5.55±0.03)×10^-9 and (38±4)×10^-9. The latter glitch is followed by an exponential-like recovery with characteristic timescale of ∼30 d. The Vela pulsar presents an under-abundance of small glitches comparatively to many other glitching pulsars, which appears genuine and not a result of observational biases. Besides typical glitches, the smooth spin down of the pulsar is also affected by an almost continuous activity that can be partially characterised by step-like changes in ν, \dot{ν} or both.

Page created on November 7, 2020.