The Persistent Radio Sources and Multi-wavelength Counterparts of Fast Radio Bursts in Massive Binary Systems

TL;DR

This paper explores the electromagnetic counterparts of fast radio bursts in massive star binaries, proposing models for persistent radio sources and bow shock radiation, and predicts their detectability across multiple wavelengths.

Contribution

It introduces a comprehensive model linking persistent radio sources and bow shock emissions to FRBs in magnetar-massive star binaries, highlighting their potential observability.

Findings

PRSs with luminosity 10^{38}-10^{39} erg/s can be produced by young magnetar wind nebulae.

Flux variations of PRSs can be explained by magnetar magnetic field decay.

Multi-wavelength emissions from bow shocks are detectable within certain distances with current instruments.

Abstract

Fast radio bursts (FRBs) are millisecond-duration pulses originating from cosmological distances. Multi-wavelength counterparts associated with FRBs are important for unveiling their physical origins. Recent observations provide strong evidence that the sources of some active FRBs are residing in massive star binaries. In this paper, we study the electromagnetic counterparts of FRBs, including the persistent radio sources (PRSs) and the bow shock radiation from wind collisions for FRBs residing in magnetar - massive star binaries. We find that the PRSs with luminosity $10^{38}-10^{39}$ erg s$^{-1}$ can be generated by young magnetar wind nebulae (MWN). The age of magnetars is a few decades. The observed long-term variation of flux density for PRSs can be explained by the internal magnetic field decay of magnetars. The bow shock radiation can account for the less luminous PRS of FRB 20201124A. The multi-wavelength emission arising from synchrotron radiation and inverse-Compton scattering in the bow shock can be the electromagnetic counterpart of FRBs. The emission at keV, GeV and TeV bands from the binary model can be detected at the distances of $\sim10-100$ Mpc, $\sim 1-10$ Mpc and $\sim0.1$ Mpc by current instruments, respectively.