论文标题
FRB周期性：紧密O/B-Star二进制
FRB-periodicity: mild pulsars in tight O/B-star binaries
论文作者
论文摘要
在两个快速无线电爆发（FRB）源中观察到的周期性（在FRB 180916中为16天。J0158+65+65和160天FRB 121102）与紧密的，出色的质量二进制系统一致。在FRB 180916.J0158+65中，主要是质量损耗率的早期Ob-type星，$ \ dot {m} \ sim 10^{ - 8} - 10^{ - 7} m_ \ odot $ yr $ yr $ yr $^{ - 1} $，以及中等的中子星星。观察到的周期性不是FRB源的固有性，而是由于轨道相位依赖于巨大恒星风中吸收条件的调节。观察到的相对狭窄的FRB活动窗口意味着，主的风动态主导着Pulsar的风，$η= l_ {sd}/（\ dot {m} v_w c）\ leq 1 $，其中$ l_ {sd} $ is pulsar spinown，pulsar spine，$ \ dot {m} $ is $ is per {m is $ is $ smass $ s Mass $ vel $ vel。条件$η\ leq 1 $需要$ l_ {sd} \ Lessim 10^{37} $ erg $ s^{ - 1} $，需要轻度强大的脉冲星。这些观察结果与磁性磁层中的磁性无线电恒星（经典磁铁）的磁层磁层中。
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 mass loss rate $\dot{M} \sim 10^{-8}- 10^{-7} M_\odot$ yr$^{-1}$, and the secondary 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, $η= L_{sd}/(\dot{M} v_w c) \leq 1$, where $L_{sd} $ is pulsar spin-down, $\dot{M}$ is the primary's wind mass loss rate and $v_w$ is its velocity. The condition $η\leq 1$ requires mildly powerful pulsar with $L_{sd} \lesssim 10^{37}$ erg $s^{-1}$. The observations are consistent with magnetically-powered radio emission originating in the magnetospheres of strongly magnetized neutron stars, the classical magnetars.
