FRB Periodicity: Mild Pulsars in Tight O/B-star Binaries
FRB Periodicity: Mild Pulsars in Tight O/B-star Binaries
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DOI：
10.3847/2041-8213/ab87a4
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发表时间：
2020-02
期刊：
影响因子：
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通讯作者：
M. Lyutikov;M. Barkov;D. Giannios
中科院分区：
文献类型：
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作者：
M. Lyutikov;M. Barkov;D. Giannios
在两个快射电爆发（FRB）源（FRB 180916.J0158+65为16天，FRB 121102为160天）中观察到的周期性与紧的恒星质量双星系统一致。在FRB 180916.J0158+65的例子中，主星是一颗早期的OB型星星，质量损失率为yr−1，而副星是一颗中子星星星。观测到的周期性并不是FRB源所固有的，而是由于大质量星星风中吸收条件的轨道相位相关调制。观测到的相对较窄的FRB活动窗口意味着主星的风在动力学上主导着脉冲星的风，其中Lsd是脉冲星自旋下降，是主星的风质量损失率，vw是其速度。条件η ≤ 1需要一个中等强度的脉冲星，其Lsd为<$1037 erg s−1。这些观测结果与起源于年轻的强磁化中子星（经典磁星）磁层的磁动力无线电发射相一致。
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 Lsd is the pulsar spin-down, is the primary’s wind mass-loss rate, and vw is its velocity. The condition η ≤ 1 requires a mildly powerful pulsar with Lsd ≲ 1037 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.