TY - JOUR
T1 - Testing the Young Neutron Star Scenario with Persistent Radio Emission Associated with FRB 121102
AU - Kashiyama, Kazumi
AU - Murase, Kohta
N1 - Funding Information:
The work of K.M. is supported by NSF grant No. PHY-1620777.
Publisher Copyright:
© 2017. The American Astronomical Society. All rights reserved.
PY - 2017/4/10
Y1 - 2017/4/10
N2 - Recently a repeating fast radio burst (FRB) 121102 has been confirmed to be an extragalactic event and a persistent radio counterpart has been identified. While other possibilities are not ruled out, the emission properties are broadly consistent with Murase et al. that theoretically proposed quasi-steady radio emission as a counterpart of both FRBs and pulsar-driven supernovae. Here, we constrain the model parameters of such a young neutron star scenario for FRB 121102. If the associated supernova has a conventional ejecta mass of Mej μ a few Mo, a neutron star with an age of tage ∼ 10-100 years, an initial spin period of Pi ≲ a few ms, and a dipole magnetic field of Bdip ≲ a few ×1013 G can be compatible with the observations. However, in this case, the magnetically powered scenario may be favored as an FRB energy source because of the efficiency problem in the rotation-powered scenario. On the other hand, if the associated supernova is an ultra-stripped one or the neutron star is born by the accretion-induced collapse with ej ∼ 0.1 o, a younger neutron star with tage ∼ 1-10 years can be the persistent radio source and might produce FRBs with the spin-down power. These possibilities can be distinguished by the decline rate of the quasi-steady radio counterpart.
AB - Recently a repeating fast radio burst (FRB) 121102 has been confirmed to be an extragalactic event and a persistent radio counterpart has been identified. While other possibilities are not ruled out, the emission properties are broadly consistent with Murase et al. that theoretically proposed quasi-steady radio emission as a counterpart of both FRBs and pulsar-driven supernovae. Here, we constrain the model parameters of such a young neutron star scenario for FRB 121102. If the associated supernova has a conventional ejecta mass of Mej μ a few Mo, a neutron star with an age of tage ∼ 10-100 years, an initial spin period of Pi ≲ a few ms, and a dipole magnetic field of Bdip ≲ a few ×1013 G can be compatible with the observations. However, in this case, the magnetically powered scenario may be favored as an FRB energy source because of the efficiency problem in the rotation-powered scenario. On the other hand, if the associated supernova is an ultra-stripped one or the neutron star is born by the accretion-induced collapse with ej ∼ 0.1 o, a younger neutron star with tage ∼ 1-10 years can be the persistent radio source and might produce FRBs with the spin-down power. These possibilities can be distinguished by the decline rate of the quasi-steady radio counterpart.
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U2 - 10.3847/2041-8213/aa68e1
DO - 10.3847/2041-8213/aa68e1
M3 - Article
AN - SCOPUS:85018522919
SN - 2041-8205
VL - 839
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 1
M1 - L3
ER -