FRB 190520B embedded in a magnetar wind nebula and supernova remnant: luminous persistent radio source, decreasing dispersion measure and large rotation measure

TL;DR

This paper models FRB 190520B as a young magnetar embedded in a magnetar wind nebula and supernova remnant, explaining its high dispersion measure, large rotation measure, and persistent radio source.

Contribution

It introduces a model where a young magnetar in a composite nebula and remnant explains multiple observed features of FRB 190520B, including DM, RM, and PRS.

Findings

The magnetar has an internal magnetic field of (2-4)×10^{16} G.

The magnetar's age is estimated at 14-22 years.

The dense supernova ejecta accounts for the high DM and RM.

Abstract

Recently, FRB 190520B with the largest extragalactic dispersion measure (DM), was discovered by the Five-hundred-meter Aperture Spherical radio Telescope (FAST). The DM excess over the intergalactic medium and Galactic contributions is estimated as $\sim 900$ pc cm$^{-3}$, which is nearly ten times higher than other fast radio bursts (FRBs) host galaxies. The DM decreases with the rate $\sim0.1$ pc cm$^{-3}$ per day. It is the second FRB associated with a compact persistent radio source (PRS). The rotation measure (RM) is found to be larger than $1.8 \times 10^{5} \mathrm{rad} ~\mathrm{m}^{-2}$. In this letter, we argue that FRB 190520B is powered by a young magentar formed by core-collapse of massive stars, embedded in a composite of magnetar wind nebula (MWN) and supernova remnant (SNR). The energy injection of the magnetar drives the MWN and SN ejecta to evolve together, and the PRS is generated by the synchrotron radiation of the MWN. The magnetar has the interior magnetic field $B_{\text{int}}\sim (2-4)\times 10^{16}$ G and the age $t_{\text{age}}\sim 14-22$ yr. The dense SN ejecta and the shocked shell contribute a large fraction of the observed DM and RM. Our model can naturally explain the luminous PRS, decreasing DM and extreme RM of FRB 190520B simultaneously.