A Real time Automated Glitch Detection Pipeline at Ooty Radio Telescope (ORT)

Pulsars being a massive and extremely dense object they have very stable rotation rate. They are rival to some of the most precise terrestrial clocks. The beamed pulsed emission from pulsars originates few hundreds of kilometres above the magnetic pole of the star and co-rotates with the stellar surface, hence the time of arrival (ToA) of the pulsed radio emission on earth carries the rotational information about the star. Pulsars are sometimes categorized by their age, a large fraction of the younger pulsars exhibit two types of rotational instabilities, one is called as pulsar glitches and the other is the timing noise, which is observed as deviations in ToAs of pulses from the expected. Pulsar glitches are sudden spin-up of the star, whereas the timing noise is due to the jittery rotation of the pulsars. The pulsars are cold system resulting in the formation of superfluid of neutrons which are responsible for glitches. The post glitch evolution of the rotation rate is observed with exponential decay, in some cases, more than a single exponential recovery has been observed, the timescales of recovery is closely connected to the in-homogeneous matter inside the neutron star crust and the properties of the superfluids.