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Superluminal motion of a relativistic jet in the neutron-star merger GW170817
Nature ( IF 64.8 ) Pub Date : 2018-09-01 , DOI: 10.1038/s41586-018-0486-3 K P Mooley 1, 2 , A T Deller 3, 4 , O Gottlieb 5 , E Nakar 5 , G Hallinan 2 , S Bourke 6 , D A Frail 1 , A Horesh 7 , A Corsi 8 , K Hotokezaka 9
Nature ( IF 64.8 ) Pub Date : 2018-09-01 , DOI: 10.1038/s41586-018-0486-3 K P Mooley 1, 2 , A T Deller 3, 4 , O Gottlieb 5 , E Nakar 5 , G Hallinan 2 , S Bourke 6 , D A Frail 1 , A Horesh 7 , A Corsi 8 , K Hotokezaka 9
Affiliation
The binary neutron-star merger GW1708171 was accompanied by radiation across the electromagnetic spectrum2 and localized2 to the galaxy NGC 4993 at a distance3 of about 41 megaparsecs from Earth. The radio and X-ray afterglows of GW170817 exhibited delayed onset4–7, a gradual increase8 in the emission with time (proportional to t0.8) to a peak about 150 days after the merger event9, followed by a relatively rapid decline9,10. So far, various models have been proposed to explain the afterglow emission, including a choked-jet cocoon4,8,11–13 and a successful-jet cocoon4,8,11–18 (also called a structured jet). However, the observational data have remained inconclusive10,15,19,20 as to whether GW170817 launched a successful relativistic jet. Here we report radio observations using very long-baseline interferometry. We find that the compact radio source associated with GW170817 exhibits superluminal apparent motion between 75 days and 230 days after the merger event. This measurement breaks the degeneracy between the choked- and successful-jet cocoon models and indicates that, although the early-time radio emission was powered by a wide-angle outflow8 (a cocoon), the late-time emission was most probably dominated by an energetic and narrowly collimated jet (with an opening angle of less than five degrees) and observed from a viewing angle of about 20 degrees. The imaging of a collimated relativistic outflow emerging from GW170817 adds substantial weight to the evidence linking binary neutron-star mergers and short γ-ray bursts.Emission from the radio counterpart of the gravitation-wave event GW170817 was powered by a wide-angle outflow at early times, but probably dominated by a narrowly collimated jet at later times.
中文翻译:
中子星合并GW170817中相对论射流的超光速运动
双中子星合并 GW1708171 伴随着跨越电磁波谱的辐射 2 并定位 2 到距地球约 41 兆秒差距的星系 NGC 4993。GW170817 的射电和 X 射线余辉显示延迟发生 4-7,随着时间的推移,发射逐渐增加(与 t0.8 成正比),在合并事件 9 后约 150 天达到峰值,然后相对快速下降 9,10。到目前为止,已经提出了各种模型来解释余辉发射,包括阻塞喷射茧4,8,11-13 和成功喷射茧4,8,11-18(也称为结构化喷射)。然而,关于 GW170817 是否成功发射了相对论喷流,观测数据仍然没有定论10、15、19、20。在这里,我们使用超长基线干涉测量法报告无线电观测。我们发现与 GW170817 相关的紧凑型无线电源在合并事件后 75 天到 230 天之间表现出超光速视运动。这种测量打破了阻塞模型和成功喷射茧模型之间的简并性,并表明,虽然早期的无线电发射是由广角外流 8(茧)提供动力的,但后期发射最有可能由高能窄准直射流(张角小于 5 度),从大约 20 度的视角观察。来自 GW170817 的准直相对论流出的成像为将双中子星合并和短 γ 射线爆发联系起来的证据增加了重要的权重。 来自引力波事件 GW170817 的无线电对应物的发射由 GW170817 的广角流出提供动力早期,
更新日期:2018-09-01
中文翻译:
中子星合并GW170817中相对论射流的超光速运动
双中子星合并 GW1708171 伴随着跨越电磁波谱的辐射 2 并定位 2 到距地球约 41 兆秒差距的星系 NGC 4993。GW170817 的射电和 X 射线余辉显示延迟发生 4-7,随着时间的推移,发射逐渐增加(与 t0.8 成正比),在合并事件 9 后约 150 天达到峰值,然后相对快速下降 9,10。到目前为止,已经提出了各种模型来解释余辉发射,包括阻塞喷射茧4,8,11-13 和成功喷射茧4,8,11-18(也称为结构化喷射)。然而,关于 GW170817 是否成功发射了相对论喷流,观测数据仍然没有定论10、15、19、20。在这里,我们使用超长基线干涉测量法报告无线电观测。我们发现与 GW170817 相关的紧凑型无线电源在合并事件后 75 天到 230 天之间表现出超光速视运动。这种测量打破了阻塞模型和成功喷射茧模型之间的简并性,并表明,虽然早期的无线电发射是由广角外流 8(茧)提供动力的,但后期发射最有可能由高能窄准直射流(张角小于 5 度),从大约 20 度的视角观察。来自 GW170817 的准直相对论流出的成像为将双中子星合并和短 γ 射线爆发联系起来的证据增加了重要的权重。 来自引力波事件 GW170817 的无线电对应物的发射由 GW170817 的广角流出提供动力早期,