arXiv 1701.048152017-01astro-ph.HE

用与FRB 121102有关的持续无线电发射测试年轻中子星情景

Testing the Young Neutron Star Scenario with Persistent Radio Emission Associated with FRB 121102

Kazumi Kashiyama, Kohta Murase

备注：: 6 pages, 2 figures, accepted for publication in ApJ letters
发表信息：: Astrophys.J. 839 (2017) L3
DOI：: 10.3847/2041-8213/aa68e1

摘要：

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和一个持续的无线电对应物已被确定。虽然不排除其他可能性，但发射特性与Murase等人（2016）在理论上提出的准稳态无线电发射作为FRB和脉冲星驱动的超新星的对应物大致一致。在这里，我们约束这样一个年轻的中子星的情况下FRB 121102的模型参数。如果相关的超新星有一个常规的喷出物质量$M_{\rm ej}\gtrsim{\rm a \ few}\ M_\odot$，一个中子星的年龄$t_{\rm age} \sim 10-100 \ \rm yrs$，初始自旋周期$P_{i} \lesssim$几毫秒，和一个偶极磁场$B_{\rm dip} \lesssim {\rm a \ few} \times 10^{13} \ \rm G$可以与观测兼容。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，或者中子星是由$M_{\rm ej} \sim 0.1 \ M_\odot$的吸积引起的坍缩产生的，那么一个年龄为$t_{\rm age} \sim 1-10$的年轻中子星可能是持久的射电源，并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。

英文摘要：

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. (2016) 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 $M_{\rm ej}\gtrsim{\rm a \ few}\ M_\odot$, a neutron star with an age of $t_{\rm age} \sim 10-100 \ \rm yrs$, an initial spin period of $P_{i} \lesssim$ a few ms, and a dipole magnetic field of $B_{\rm dip} \lesssim {\rm a \ few} \times 10^{13} \ \rm G$ 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 $M_{\rm ej} \sim 0.1 \ M_\odot$, a younger neutron star with $t_{\rm age} \sim 1-10$ yrs 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.

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