The Thousand-Pulsar-Array programme on MeerKAT -- VIII. The subpulse modulation of 1198 pulsars

TL;DR

This study analyzes subpulse modulation in 1198 pulsars using MeerKAT, revealing a V-shaped evolution of modulation periods with pulsar age and providing insights into the underlying physics of pulsar emission mechanisms.

Contribution

It presents the largest detailed analysis of subpulse modulation properties across a wide pulsar population, uncovering the evolution pattern of modulation periods and proposing a model involving beat phenomena.

Findings

35% of pulsars exhibit drifting subpulses, more common near the deathline.

Modulation period P3 shows a V-shaped evolution with pulsar age, with the shortest periods at intermediate ages.

Identified correct periods and spin-down rates for 12 pulsars with previously ambiguous data.

Abstract

We report on the subpulse modulation properties of 1198 pulsars using the Thousand-Pulsar-Array programme on MeerKAT. About 35% of the analysed pulsars exhibit drifting subpulses which are more pronounced towards the deathline, consistent with previous studies. We estimate that this common phenomenon is detectable in 60% of the overall pulsar population if high quality data were available for all. This large study reveals the evolution of drifting subpulses across the pulsar population in unprecedented detail. In particular, we find that the modulation period $P_3$ follows a V-shaped evolution with respect to the characteristic age $\tau_c$, such that the smallest $P_3$ values, corresponding to the Nyquist period $P_3>\sim2$, are found at $\tau_c>\sim10^{7.5}$ yr. The V-shaped evolution can be interpreted and reproduced if young pulsars possess aliased fast intrinsic $P_3$, which monotonically increase, ultimately achieving a slow unaliased $P_3$. Enhancement of irregularities in intrinsic subpulse modulation by aliasing in small $\tau_c$ pulsars would explain their observed less well defined $P_3$'s and weaker spectral features. Modelling these results as rotating subbeams, their circulation must slow down as the pulsar evolves. This is the opposite to that expected if circulation is driven by ExB drift. This can be resolved if the observed $P_3$ periodicity is due to a beat between an ExB system and the pulsar period. As a by-product, we identify the correct periods and spin-down rates for 12 pulsars, for which harmonically related values were reported in the literature.