On the origin of the scatter broadening of fast radio burst pulses and astrophysical implications

TL;DR

This paper investigates the origins of scatter broadening in fast radio burst pulses, proposing models of electron density fluctuations in the intergalactic medium and host galaxies, and discusses astrophysical implications for turbulence and magnetic fields.

Contribution

It introduces a model where short-wave-dominated turbulence in host galaxies explains FRB pulse broadening, linking turbulence properties to observed scattering timescales.

Findings

Short-wave turbulence in host galaxies can account for FRB scattering.

Host galaxy turbulence influences the scaling of scattering time with DM.

Sheet-like density structures do not produce strong scattering.

Abstract

Fast radio bursts (FRBs) have been identified as extragalactic sources which can make a probe of turbulence in the intergalactic medium (IGM) and their host galaxies. To account for the observed millisecond pulses caused by scatter broadening, we examine a variety of possible models of electron density fluctuations in both the IGM and the host galaxy medium. We find that a short-wave-dominated power-law spectrum of density, which may arise in highly supersonic turbulence with pronounced local dense structures of shock-compressed gas in the host interstellar medium (ISM), can produce the required density enhancements at sufficiently small scales to interpret the scattering timescale of FRBs. It implies that an FRB residing in a galaxy with efficient star formation in action tends to have a broadened pulse. The scaling of the scattering time with dispersion measure (DM) in the host galaxy varies in different turbulence and scattering regimes. The host galaxy can be the major origin of scatter broadening, but contribute to a small fraction of the total DM. We also find that the sheet-like structure of density in the host ISM associated with folded magnetic fields in a viscosity-dominated regime of magnetohydrodynamic (MHD) turbulence cannot give rise to strong scattering. Furthermore, valuable insights into the IGM turbulence concerning the detailed spatial structure of density and magnetic field can be gained from the observed scattering timescale of FRBs. Our results are in favor of the suppression of micro-plasma instabilities and the validity of collisional-MHD description of turbulence properties in the collisionless IGM.