Measurement of the Breaking Indices of Frequently Ghtching Pulsars using Integration Method

Pulsars are old, stellar objects that emit electromagnetic radiations in a definite time interval, with a predictable smooth spin-down, predisposed to discrete fluctuations/glitches. The rotational frequency of pulsars decays with time as quantified by the breaking index which is now known to have no consequence on other pulsar qualities like obliquity angle evolution or complex high-order multiple structures but rather on its spin proportion. In the canonical model n=3, but observationally n≠3 in numerous cases. Showing that the canonical model requires modification. Using the Australian Telescope National Facility (ATNF). Pulsars catalog, we selected 208 pulsars with 670 glitches. We computed the breaking and observed that the breaking index is smaller for very young pulsars, which usually glitch more frequently than their older, more stable counterpart analysis. They have switched over from time and also account for over 68% of the entire glitches in our population. A regression analysis shows that spin properties of pulsars are ≥ 65% correlated with breaking index (n). Implications of this result are discussed.