2017/02/28 by Shota Kisaka, Teruaki Enoto, Shinpei Shibata
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics #Detector #Fast radio burst #Flare #Flux (metallurgy) #Galaxy #Gamma-ray bursts and supernovae #Luminosity #Neutron star #Optics #Physics #Pulsar #Pulsars and Gravitational Waves Research #Pulse (music) #Spin (aerodynamics) #astro-ph.HE
paper · pdf · doi:10.1093/pasj/psx093
12 pages, 1 figure. Accepted for publication in PASJ
arxiv created 2017/08/17 · openalex publication_date 2017/08/21 · arxiv updated 2017/12/20 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract Recent localization of the repeating fast radio burst (FRB) 121102 revealed the distance of its host galaxy and luminosities of the bursts. We investigated constraints on the young neutron star (NS) model, that (a) the FRB intrinsic luminosity is supported by the spin-down energy, and (b) the FRB duration is shorter than the NS rotation period. In the case of a circular cone emission geometry, conditions (a) and (b) determine the NS parameters within very small ranges, compared with that from only condition (a) discussed in previous works. Anisotropy of the pulsed emission does not affect the area of the allowed parameter region by virtue of condition (b). The determined parameters are consistent with those independently limited by the properties of the possible persistent radio counterpart and the circumburst environments such as surrounding materials. Since the NS in the allowed parameter region is older than the spin-down timescale, the hypothetical GRP (giant radio pulse)-like model expects a rapid radio flux decay of ≲1 Jy within a few years as the spin-down luminosity decreases. The continuous monitoring will provide constraints on the young NS models. If no flux evolution is seen, we need to consider an alternative model, e.g., the magnetically powered flare.