Emission from a Pulsar Wind Nebula: Application to the Persistent Radio Counterpart of FRB 121102. (arXiv:1911.12833v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Yang_Y/0/1/0/all/0/1">Yu-Han Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dai_Z/0/1/0/all/0/1">Zi-Gao Dai</a>
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.
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.
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