期刊
ASTROPHYSICAL JOURNAL LETTERS
卷 893, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.3847/2041-8213/ab87a4
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资金
- NASA [80NSSC17K0757]
- NSF [10001562, 10001521]
Periodicities observed in two fast radio burst (FRB) sources (16 days in FRB 180916.J0158+65 and 160 days in FRB 121102) are consistent with that of tight, stellar-mass binary systems. In the case of FRB 180916.J0158+65 the primary is an early OB-type star with the mass-loss rate yr(-1), and the secondary is a neutron star. The observed periodicity is not intrinsic to the FRB's source, but is due to the orbital phase-dependent modulation of the absorption conditions in the massive star's wind. The observed relatively narrow FRB activity window implies that the primary's wind dynamically dominates that of the pulsar,, where L-sd is the pulsar spin-down, is the primary's wind mass-loss rate, and v(w) is its velocity. The condition eta <= 1 requires a mildly powerful pulsar with L-sd less than or similar to 10(37) erg s(-1). The observations are consistent with magnetically powered radio emission originating in the magnetospheres of young, strongly magnetized neutron stars, the classical magnetars.
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