发表机构
University of Pisa; INFN - Pisa; INAF - Osservatorio Astronomico di Roma; INAF - Osservatorio Astronomico di Brera; Universität Heidelberg, Zentrum für Astronomie (ZAH), Institut für Theoretische Astrophysik; Universität Heidelberg, Interdisziplinäres Zentrum für Wissenschaftliches Rechnen; University of Padova; INFN, Sezione di Padova（比萨大学; 意大利国家核物理研究所-比萨分部; 意大利国家天体物理研究所罗马天文台; 意大利国家天体物理研究所布里埃拉天文台; 海德堡大学天文学中心理论天体物理研究所; 海德堡大学跨学科科学计算中心; 帕多瓦大学; 意大利国家核物理研究所帕多瓦分部）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过对比合成双中子星并合及相关快速射电暴群体的探测率与CHIME观测率，发现双中子星并合及其中产生的磁星可解释部分快速射电暴，为多信使天文学提供了支撑。
AI 中文摘要
快速射电暴（Fast Radio Bursts, FRBs）是具有毫秒量级持续时间的高能射电源，其物理起源至今仍不明确。许多模型认为磁星是FRBs的可能起源体，这一观点得到了FRB与银道面磁星SGR 1935+2154成协的支持；其他被提出的起源体还包括双中子星（binary neutron star, BNS）并合，而BNS并合本身与磁星的形成相关。本研究通过将合成BNS及相关FRB群体推导得到的探测率与CHIME观测到的率进行比较，探究FRBs与BNS并合（包括这类事件中可能产生的磁星）之间的潜在联系。我们结合近期从理论上预测的BNS并合率随红移的变化关系，以及从银道面BNS测量中推断出的中子星质量分布，生成了一份BNS并合的合成星表。利用该星表，我们针对不同的物态方程，预测了以磁星（稳定或超大质量中子星）或黑洞（即时形成或在超大质量中子星坍缩后形成）终结的BNS系统数量。随后，我们为每个BNS（因此也为每个磁星残余体）模拟了一个相关的FRB，并估算了其中有多少个可能被CHIME探测到。我们发现，BNS并合率以及BNS后产生的磁星率在CHIME探测到的FRBs（包括重复和非重复FRBs）中占比不可忽略。尽管需要考虑额外的形成通道以解释全部FRB群体，但部分FRBs可能确实与BNS并合成协的这一发现，在多信使天文学领域具有深远意义，支持利用当前及未来设备系统地搜寻FRBs与BNS并合产生的引力波（GW）的成协探测。
英文摘要
Fast Radio Bursts (FRBs) are highly energetic radio sources whose duration is of the order of milliseconds. The physical origin of these sources is still unknown. Many models suggest magnetars as possible progenitors of FRBs, and this is supported by the association between FRBs and the Galactic magnetar SGR 1935+2154; other proposed progenitors include binary neutron star (BNS) mergers, that are themselves linked to magnetar formation. In this work we investigate the possible connection between FRBs and BNS mergers, including magnetars that might be produced in such events, by comparing the detection rates inferred from synthetic BNS and associated FRB populations with the rates observed by CHIME. We produce a synthetic catalog of BNS mergers by combining recent theoretically predicted BNS merger rate as a function of redshift and the neutron star mass distribution inferred from measurements of Galactic BNSs. Using this catalog we predict the number of BNS systems ending as magnetars (stable or supramassive neutron star) or black holes (formed promptly or after the collapse of a hypermassive neutron star) for different equations of state. We then simulate for each BNS (and therefore for each magnetar remnant) an associated FRB and estimate how many of them can be potentially detected by CHIME. We find that the rate of BNS mergers and the rate of magnetars produced after BNS represents a non-negligible fraction of the FRBs detected by CHIME, both repeating and non-repeating. Although additional formation channels need to be considered to account for the entire population of FRBs, the existence of a fraction of FRBs that might genuinely be associated to BNS mergers has profound implications in the context of multi- messenger astronomy, supporting the systematic searches of coincident detections of FRBs and GWs from a BNS merger with current and future facilities.
Comments5 pages. Accepted for publication in A&A
