论文标题

来自二进制中子星星合并的无线电余星的可检测性及其对快速无线电爆发的影响

Detectability of radio afterglows from binary neutron star mergers and implications for fast radio bursts

论文作者

Lin, Haoxiang, Totani, Tomonori

论文摘要

二进制中子星(BNS)合并是重复和非重复的快速无线电爆发(FRB)的拟议起源之一,它将FRB与引力波和短伽马射线爆发(GRBS)相关联。在这项工作中,我们探索了来自BNS合并的无线电余波的可检测性,并将其与FRB余气上观察到的无线电限制进行比较。我们计算由两个组件提供动力的余辉通量:相对论射流和较慢的各向同性喷射,并量化检测概率是源红移的函数,观察时间和磁通敏感性。采用了从短GRB余波推断出的模型参数分布,并假定视角分布(均匀的球形,重力波,轴心上的轴心)反映了不同的搜索场景。假设FRB不强烈,我们将与报告的无线电限制检测到的FRB进行比较,并发现检测概率通常为1---10%,因此考虑到小样本数量的BNS祖细胞模型(<10),对BNS祖细胞模型没有很大的限制。特别是对于附近的一些FRB(例如180916.J0158+65,190608),我们发现对$ \ sim $ \ sim $ \ sim $ \ sim $ \ sim $ \ sim $ 1--10 $ 1--10年,我们发现很有可能被检测到很高的检测(> 20%,> 20%,为10 $μ$ jy jy敏感性)。因此,对这些对象的持续无线电发射的长期无线电监视很重要。

Binary neutron star (BNS) mergers are one of the proposed origins for both repeating and non-repeating fast radio bursts (FRBs), which associates FRBs with gravitational waves and short gamma-ray bursts (GRBs). In this work, we explore detectability of radio afterglows from BNS mergers and compare it to the observed radio limits on FRB afterglows. We calculate the afterglow flux powered by the two components: a relativistic jet and a slower isotropic ejecta, and quantify the detection probability as a function of the source redshift, observing time, and flux sensitivity. The model parameter distributions inferred from short GRB afterglows are adopted, and viewing angle distributions (uniform spherical, gravitational-wave, on-axis biased) are assumed to reflect different searching scenario. Assuming that FRBs are not strongly beamed, we make comparison to FRBs detected with reported radio limits and find the detection probabilities are 1--10% in general, and hence not a strong constraint on the BNS progenitor model considering the small sample number (<10). In particular for some nearby FRBs (e.g. 180916.J0158+65, 190608), we find a high chance of detection (>20% at 10$μ$Jy sensitivity) for the isotropic component that would peak around $\sim$1--10 years after the merger. Therefore a long term radio monitoring of persistent radio emission for these objects is important.

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