Emission from a Pulsar Wind Nebula: Application to the Persistent Radio Counterpart of FRB 121102

Abstract

The properties of fast radio bursts (FRBs) indicate that the physical origin of this type of astrophysical phenomenon is related to neutron stars. The first detected repeating source, FRB 121102, is associated with a persistent radio counterpart. In this paper, we propose that this radio counterpart could arise from a pulsar wind nebula powered by a magnetar without surrounding supernova ejecta. Its medium is a stratified structure produced by a progenitor wind. The model parameters are constrained by the spectrum of the counterpart emission, the size of the nebula, and the large but decreasing rotation measure (RM) of the repeating bursts. In addition, the observed dispersion measure is consistent with the assumption that all of the RM comes from the shocked medium.

arXiv comment10 pages, 4 figures, 1 table. Published in the Astrophysical Journal on Nov. 11, 2019

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Cited by in corpus (14)

• Are persistent emission luminosity and rotation measure of fast radio bursts related?
• Binary comb models for FRB 121102
• Radio emission from a decade old Type I superluminous supernova, PTF10hgi: Comparison with FRB121102
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• Fast radio bursts as strong waves interacting with ambient medium
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• Quasi-steady emission from repeating fast radio bursts can be explained by magnetar wind nebulae
• Milliarcsecond-scale spectrum of the persistent radio source associated with FRB 20190417A and constraints for FRB 20181030A
• A Generic Model for Persistent Radio Source around Fast Radio Bursts
• FRB 190520B embedded in a magnetar wind nebula and supernova remnant: luminous persistent radio source, decreasing dispersion measure and large rotation measure