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.
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science