论文标题
我们能否约束用短伽马射线爆发的二进制中子星合并的后果？
Can we constrain the aftermath of binary neutron star mergers with short gamma-ray bursts?
论文作者
论文摘要
GW170817和GRB170817A的联合观察证明，二进制中子星（BNS）合并是短伽马射线爆发（SGRB）的祖先：这建立了仍未设定的SGRB中央发动机与BNS Mergger sate of Seation os nouts nouts Antemes and Nate and Nate and Nate and Nate and nate and Nate的直接联系（SGRB）的直接联系。我们提出了一种基于此链接的SGRB的中心发动机的新方法。我们通过将最新的理论预测的BNS合并率与红移的函数和从银河BNS的测量值相结合，从而产生BNS合并的扩展目录。我们使用此目录来预测以磁铁（稳定或超质量NS）或BHS（迅速形成或过度量NS崩溃后形成）结尾的BNS系统的数量，我们将这些结果与观察到的SGRB进行了比较。尽管不确定性主要与SGRB射流结构的知识不足有关，但我们发现，对于大多数EOSS，BNS合并后产生的磁铁速率足以为所有SGRB提供动力，而仅使用BHS的场景只是中央发动机的情况似乎消除了。
The joint observation of GW170817 and GRB170817A proved that binary neutron star (BNS) mergers are progenitors of short Gamma-ray Bursts (SGRB): this established a direct link between the still unsettled SGRB central engine and the outcome of BNS mergers, whose nature depends on the equation of state (EOS) and on the masses of the NSs. We propose a novel method to probe the central engine of SGRBs based on this link. We produce an extended catalog of BNS mergers by combining recent theoretically predicted BNS merger rate as a function of redshift and the NS mass distribution inferred from measurements of Galactic BNSs. We use this catalog to predict the number of BNS systems ending as magnetars (stable or Supramassive NS) or BHs (formed promptly or after the collapse of a hypermassive NS) for different EOSs, and we compare these outcomes with the observed rate of SGRBs. Despite the uncertainties mainly related to the poor knowledge of the SGRB jet structure, we find that for most EOSs the rate of magnetars produced after BNS mergers is sufficient to power all the SGRBs, while scenarios with only BHs as possible central engine seems to be disfavoured.
