Testing the Young Neutron Star Scenario with Persistent Radio Emission Associated with FRB 121102
Testing the Young Neutron Star Scenario with Persistent Radio Emission Associated with FRB 121102
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DOI：
10.3847/2041-8213/aa68e1
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发表时间：
2017-01
期刊：
影响因子：
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通讯作者：
K. Kashiyama;K. Murase
中科院分区：
文献类型：
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作者：
K. Kashiyama;K. Murase
最近，一个重复的快速射电暴（FRB）121102已被证实是一个河外事件，并已确定了一个持久的无线电对应物。虽然不排除其他可能性，但发射性质与村濑等人的理论大致一致，他们提出准稳态射电发射是FRB和脉冲星驱动的超新星的对应物。在这里，我们约束这样一个年轻的中子星星的情况下FRB 121102的模型参数。如果相关超新星的常规喷出物质量为Mej =几个M，那么年龄为10-100年，初始自旋周期为π =几个ms，偶极磁场为Bdip =几个× 10 ~（13）G的中子星星就可以与观测结果相符合。然而，在这种情况下，由于旋转供能方案中的效率问题，磁供能方案可以作为FRB能量源而受到青睐。另一方面，如果关联的超新星是一个超剥离的超新星，或者中子星星是由Mej为0.1 M的吸积引起的坍缩而产生的，那么年龄为1.1 -10年的年轻中子星星可能是持久的射电源，并且可能产生具有下旋功率的FRB。这些可能性可以通过准稳态无线电对应物的下降率来区分。
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 Murase et al. that theoretically proposed quasi-steady radio emission as a counterpart of both FRBs and pulsar-driven supernovae. 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 Mej ≳ a few M⊙, a neutron star with an age of tage ∼ 10–100 years, an initial spin period of Pi ≲ a few ms, and a dipole magnetic field of Bdip ≲ a few × 1013 G can be compatible with the observations. However, in this case, the magnetically powered scenario may be 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 or the neutron star is born by the accretion-induced collapse with Mej ∼ 0.1 M⊙, a younger neutron star with tage ∼ 1–10 years can be the persistent radio source and might produce FRBs with the spin-down power. These possibilities can be distinguished by the decline rate of the quasi-steady radio counterpart.