Testing Models of Periodically Modulated FRB Activity

重新审视FRB 20201124A报告的周期使用MCMC方法

Revisiting the Reported Period of FRB 20201124A Using MCMC Methods

本文提出结合相位折叠和MCMC参数估计的方法，用于快速重复FRB的周期搜索，验证了该方法能有效恢复已报告的候选周期。

FRB 20180916B周期活动的物理起源

The physical origin of the periodic activity for FRB 20180916B

针对FRB 20180916B的16天周期活动起源之谜，研究通过观测数据研判发现超长自转模型最可能但无法解释RM变化，进而提出含慢转中子星的大质量双星自洽模型，其RM周期性可由未来观测检验。

A Neutron Star-White Dwarf Binary Model for Periodically Active Fast Radio Burst Sources

We propose a compact binary model with an eccentric orbit to explain periodically active fast radio burst (FRB) sources, where the system consists of a neutron star (NS) with strong dipolar magnetic fields and a magnetic white dwarf (WD). In our model, the WD fills its Roche lobe at periastron, and mass transfer occurs from the WD to the NS around this point. The accreted material may be fragmented into a number of parts, which arrive at the NS at different times. The fragmented magnetized material may trigger magnetic reconnection near the NS surface. The electrons can be accelerated to an ul…

The spectral properties of the bright FRB population

We examine the spectra of 23 fast radio bursts detected in a fly's-eye survey with the Australian SKA Pathfinder, including those of three bursts not previously reported. The mean spectral index of $α= -1.6_{-0.2}^{+0.3}$ ($F_ν\propto ν^α$) is close to that of the Galactic pulsar population. The sample is dominated by bursts exhibiting a large degree of spectral modulation: 17 exhibit fine-scale spectral modulation with an rms exceeding 50% of the mean, with decorrelation bandwidths (half-maximum) ranging from $\approx$ to 49 MHz. Most decorrelation bandwidths are an order of magnitude lower t…

Orbit-induced spin precession as an origin of periodicity in periodically-repeating fast radio bursts

FRB 180916.J0158+65 has been found to repeatedly emit fast radio bursts with the period in roughly 16 days. We propose that such periodicity comes from orbit-induced, spin precession of the emitter, which is possibly a neutron star. Depending on the mass of the companion, the binary period ranges from several hundred to thousands of seconds. Such tight binaries have a relatively short lifetime, which does not likely come from the gravitational decay of a wide binary. We comment on the relation to GW190425 and the possibility in LISA and LIGO detections.

Periodic activity from fast radio burst FRB180916 explained in the frameof the orbiting asteroid model

Observation of fast radio bursts (FRBs) are rising very quickly with the advent of specialised instruments and surveys, and it has recently been shown that some of them repeat quasi-periodically. In particular, evidence of a $P=16.35$ day period has been reported for FRB 180916.J0158+65. We seek an explanation within the frame of our orbiting asteroid model, whereby FRBs are produced in the plasma wake of asteroids immersed in the wind of a pulsar or a magnetar. We used the data reported by the CHIME/FRB collaboration in order to infer the orbital characteristics of asteroid swarms, and perfor…