Speaker
Description
The sudden increase in the spin frequency of a pulsar, known as a pulsar glitch, provides valuable insights into the dynamics of matter within neutron stars. Glitches are believed to occur because of the transfer of angular momentum within the neutron star’s interior, which accumulates over time due to the motion of its components. If the source of this
transferred momentum is depleted during a glitch event, the glitch size can determine when the next event will occur – this is known as the momentum reservoir effect. Traditionally, researchers have looked for this effect by examining the relationship between glitch size and the time interval between glitches. However, in our analysis, we took a different approach by examining the relationship between the glitch size and the number of rotations the pulsar undergoes between glitches. After employing Bayesian inference, our results exposed a stronger correlation compared to the traditional approach. Our results imply that, the number of rotations may influence the amount of angular momentum transferred during a glitch. We also noted that the traditional approach did not consider the rotation lag as a function of pulsar spin frequency, suggesting that the number of rotations may be a better way to study the reservoir effect on glitch sizes. Our innovative approach sheds more light on the complex interplay between superfluid and normal matter and enhances predictions of glitch events, informing multimessenger astronomy. Based on this observation, we shall model the moment of inertia of the superfluid component, and distributions with respect to the recovery time to ascertain possible connection.
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