Long-term timing and emission behavior of the young Crab-like pulsar PSR B0540-69

TL;DR

This study provides detailed timing analysis of the young pulsar PSR B0540-69 over 15.8 years, revealing a second glitch, a consistent braking index, and stable emission, highlighting differences from the Crab pulsar and variability among young neutron stars.

Contribution

It presents the first detection of a second glitch in PSR B0540-69 and offers a comprehensive timing and emission analysis over a long-term dataset.

Findings

Detected a second glitch at MJD 52927 with specific fractional changes.

Measured a consistent braking index of approximately 2.129.

Found no significant flux or pulse profile variations.

Abstract

We present timing solutions and spin properties of the young pulsar PSR B0540-69 from analysis of 15.8 yr of data from the Rossi X-Ray Timing Explorer. We perform a partially phase-coherent timing analysis in order to mitigate the pronounced effects of timing noise in this pulsar. We also perform fully coherent timing over large subsets of the data set in order to arrive at a more precise solution. In addition to the previously reported first glitch undergone by this pulsar, we find a second glitch, which occurred at MJD 52927 $\pm$ 4, with fractional changes in spin frequency $\Delta\nu/\nu = (1.64 \pm 0.05) \times 10^{-9}$ and spin-down rate $\Delta\dot{\nu}/\dot{\nu} = (0.930 \pm 0.011) \times 10^{-4}$ (taken from our fully coherent analysis). We measure a braking index that is consistent over the entire data span, with a mean value $n = 2.129 \pm 0.012$, from our partially coherent timing analysis. We also investigated the emission behavior of this pulsar, and have found no evidence for significant flux changes, flares, burst-type activity, or pulse profile shape variations. While there is strong evidence for the much-touted similarity of PSR B0540-69 to the Crab pulsar, they nevertheless differ in several aspects, including glitch activity, where PSR B0540-69 can be said to resemble certain other very young pulsars. It seems clear that the specific processes governing the formation, evolution, and interiors of this population of recently born neutron stars can vary significantly, as reflected in their observed properties.