http://arxiv.org/abs/1701.04815
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 theoretical suggestions of Murase et al. (2016) for quasi-steady nebula emission from a pulsar-driven supernova remnant as a counterpart of FRBs. 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 $M_{\rm ej}\gtrsim{\rm a \ few}\ M_\odot$, a neutron star with an age of $t_{\rm age} \sim 10-100 \ \rm yrs$, an initial spin period of $P_{\rm i} \lesssim$ a few ms, and a dipole magnetic field of $B_{\rm dip} \sim 10^{12-13} \ \rm G$ can be compatible with the observations. However, in this case, the magnetically-powered scenario may be more 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 with $M_{\rm ej} \sim 0.1 \ M_\odot$, a younger neutron star with $t_{\rm age} \sim 1-10$ yrs can be the persistent radio source and might produce FRBs with the spin-down power. These possibilities could be distinguished by the decline rate of the quasi-steady radio counterpart.
K. Kashiyama and K. Murase
Wed, 18 Jan 17
4/61
Comments: 6 pages, 2 figures
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