论文标题
使用H.E.S.S.探测GW170817中的磁场观察
Probing the magnetic field in the GW170817 outflow using H.E.S.S. observations
论文作者
论文摘要
第一个电磁对应物与二进制中子星(BNS)合并GW170817的检测建立了短$γ$ ray爆发与BNS合并之间的联系。它还通过R过程中的核合成中的射出(所谓的Kilonova)中的重元素(所谓的Kilonova)锻造。持续了超过100天的非热收音机和X射线发射以及亮度的出现是出乎意料的。当前的理论模型试图解释这种时间行为,因为源自相对论的离轴喷射或类似Kilonova的流出。在这两种情况下,对于在非热电子中与发射区域的磁场相比,在非热电子中运输了多少能量。将VLA(无线电)和Chandra(X射线)测量与GEV-TEV域中的观察结果相结合可以帮助打破这种歧义,几乎独立于假定的发射起源。在这里,我们首次在深H.E.S.S.在BNS与完整的H.E.S.S.合并后的124至272天之间,GW170817 / GRB 170817A的观察结果。望远镜阵列以及对提示(<5天)观察的更新分析,并使用已升级的H.E.S.S. I期望远镜。我们讨论H.E.S.S.的含义在不同源场景的情况下,磁场的测量。
The detection of the first electromagnetic counterpart to the binary neutron star (BNS) merger remnant GW170817 established the connection between short $γ$-ray bursts and BNS mergers. It also confirmed the forging of heavy elements in the ejecta (a so-called kilonova) via the r-process nucleosynthesis. The appearance of non-thermal radio and X-ray emission, as well as the brightening, which lasted more than 100 days, were somewhat unexpected. Current theoretical models attempt to explain this temporal behavior as either originating from a relativistic off-axis jet or a kilonova-like outflow. In either scenario, there is some ambiguity regarding how much energy is transported in the non-thermal electrons versus the magnetic field of the emission region. Combining the VLA (radio) and Chandra (X-ray) measurements with observations in the GeV-TeV domain can help break this ambiguity, almost independently of the assumed origin of the emission. Here we report for the first time on deep H.E.S.S. observations of GW170817 / GRB 170817A between 124 and 272 days after the BNS merger with the full H.E.S.S. array of telescopes, as well as on an updated analysis of the prompt (<5 days) observations with the upgraded H.E.S.S. phase-I telescopes. We discuss implications of the H.E.S.S. measurement for the magnetic field in the context of different source scenarios.