Timing results of 22 years for PSR J0922+0638

TL;DR

This 22-year study of PSR J0922+0638 reveals a small unreported glitch, multiple slow glitches, and periodic timing noise variations, enhancing understanding of pulsar rotational irregularities.

Contribution

The paper reports the discovery of a previously unreported small glitch, multiple slow glitches, and periodic timing noise variations in PSR J0922+0638 over 22 years, providing new insights into pulsar timing irregularities.

Findings

Discovered a small glitch at MJD ~53325 with a frequency jump of ~0.79e-9.

Detected ten slow glitches occurring quasi-periodically every ~553 days.

Identified a change in the spectral index of timing noise before and after the large glitch.

Abstract

We conducted a timing analysis of PSR J0922+0638 (B0919+06) using data from the Nanshan 26 m radio telescope and the MeerKAT telescope, spanning from January 2001 to March 2023. During this 22-year period, we discovered a previously unreported small glitch (glitch 1) before the well-known large glitch (glitch 2), occurring at ${\rm MJD} \sim 53325(3)$, with a frequency jump amplitude of $\Delta \nu/\nu \sim 0.79(6) \times 10^{-9}$. We also identified ten slow glitch events, half of which were newly detected. These slow glitches occurred quasi-periodically, with an average interval of approximately 553(21) days, fractional frequency changes ranging from $\Delta \nu/\nu \sim 1.13(1) \times 10^{-9}$ to $4.08(5) \times 10^{-9}$, and a maximum fractional change in the first derivative of the frequency of $\Delta \dot{\nu}/\dot{\nu} \sim -4.6 \times 10^{-3}$. Additionally, our timing noise analysis reveals a change in the spectral index for noise power before and after glitch 2, with values of $-6.0$ and $-5.3$, respectively, likely due to this large glitch. Throughout the entire observation period, the first derivative of the spin frequency ($\dot{\nu}$) showed a periodic structure. The possible modulation period was estimated to be 537(24) days before the 700-day data gap at MJD 56716 and 600(58) days afterward. We discuss the periodic oscillations in pulsar rotation as a possible manifestation of spin-down noise and quasi-periodic slow glitches.