Abstract
Abstract Fast radio bursts (FRBs) are mysterious radio transients with millisecond durations. Recently, ∼16 days of periodic activity and ∼159 days of possible periodicity were detected to arise from FRB 180916.J0158+65 and FRB 121102, respectively, and the spin period of a slow-rotation magnetar was further considered to be one of the possible explanations of the periodic activities of repeating FRBs. For isolated neutron stars, the spin evolution suggests that it has difficulty reaching several hours. In this work, we mainly focus on the possible maximum spin period of isolated NSs/magnetars dominated by an interaction between a star’s magnetic field and the disk. We find that the disk wind plays an important role in spin evolution, whose influence varies the power-law index in the evolution equation of mass flow rate. For a magnetar without disk wind, the longest spin period is tens of hours. When the disk wind with a classical parameter is involved, the maximum spin period can reach hundreds of hours. But for an extremely large index of mass flow rate due to disk wind or other angular momentum extraction processes, a spin period of ∼(16–160) days is still possible.
Highlights
Fast radio bursts (FRBs) are radio transients with millisecond durations and extremely high brightness temperatures
From the geometrical feature, a slim disk is more likely to generate disk wind than a thin disk, but its lifetime11 is very short, i.e., even if the disk wind were strong in the slim disk phase, it could be ignored
We explore the possibly longest spin period of an isolated NS interacting with a fallback disk with and without disk wind to explain the periodic activity of FRB 180916
Summary
Fast radio bursts (FRBs) are radio transients with millisecond durations and extremely high brightness temperatures. The “close-in” models proposed that FRBs are emitted from the magnetosphere of an NS due to internal triggers (e.g., Kumar et al 2017; Lyutikov 2017; Katz 2018b; Lu & Kumar 2018; Yang & Zhang 2018; Wadiasingh & Timokhin 2019; Kumar & Bošnjak 2020; Lu et al 2020; Lyubarsky 2020; Lyutikov & Popov 2020; Wadiasingh et al 2020; Wang 2020; Wang et al 2020; Yang et al 2020) or external triggers
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