Hyper-active repeating fast radio bursts from rotation modulated starquakes on magnetars

TL;DR

This paper proposes a model combining starquake dynamics and magnetar rotation to explain the observed bimodal waiting time distribution and lack of periodicity in hyper-active repeating FRBs, aligning with observational data.

Contribution

It introduces a novel model integrating earthquake-like starquakes and magnetar rotation to explain FRB timing and energy distributions, addressing previous challenges in FRB periodicity detection.

Findings

Starquake events modulated by magnetar rotation explain bimodal waiting times.

Model accounts for non-detection of periodicity in hyper-active FRBs.

Differences in FRB properties are linked to magnetar geometric parameters.

Abstract

The non-detection of periodicity related to rotation challenges magnetar models for fast radio bursts (FRBs) with FRB emission from close to the magnetar surface. Moreover, a bimodal distribution of the burst waiting times is widely observed in hyper-active FRBs, a significant deviation from the exponential distribution expected from stationary Poisson processes. By combining the epidemic-type aftershock sequence (ETAS) earthquake model and the rotating vector model (RVM) involving the rotation of the magnetar and orientations of the spin and magnetic axes, we find that starquake events modulated by the rotation of FRB-emitting magnetar can explain the bimodal distribution of FRB waiting times, as well as the non-detection of periodicity in hyper-active repeating FRBs. We analyze data from multiple FRB sources, demonstrating that differences in waiting time distributions and, to some extent, observed energies can be explained by varying parameters related to geometric properties of the magnetar FRB emission and starquake dynamics. Our results show that the assumption that all FRBs are repeaters is compatible with our model. Notably, we find that hyper-active repeaters tend to have small magnetic inclination angles in order to hide their periodicity. We also show that our model can reproduce the waiting time distribution of a pulsar phase of the galactic magnetar SGR J1935+2154 with a larger inclination angle than the hyper-active repeaters, which could explain the detection of spin period and the relatively low observed energy for FRBs from the magnetar. The spin periods of hyper-active repeaters are not well constrained, but most likely fall in the valley region between the two peaks of the waiting time distributions.