Collaborative research: WoU-MMA: Electrodynamics of Magnetospheric Interactions in Merging Neutron Star Binaries

合作研究：WoU-MMA：合并中子星双星中磁层相互作用的电动力学

基本信息

批准号：
1908590
负责人：
Maxim Lyutikov
金额：
$ 27.06万
依托单位：
Purdue University
依托单位国家：
美国
项目类别：
Standard Grant
财政年份：
2019
资助国家：
美国
起止时间：
2019-09-01 至 2023-08-31
项目状态：
已结题

来源：
https://www.nsf.gov/awardsearch/showAward?AWD_ID=1908590&HistoricalAwards=false
关键词：
Collaborative research WoU MMA Electrodynamics

项目摘要

The detection of gravitational waves from the merger of two neutron stars in August 2017 was a seminal event for astrophysics. This amalgamation of two extremely dense former stars was associated with a short gamma-ray burst (GRB), making it clear that a merger provides the central engine of the short-duration class of this extraordinarily bright type of astrophysical explosion. In order to better understand how a neutron star merger produces a short GRB, a research collaboration between Purdue University and Princeton University will carry out theoretical and numerical investigations of the merger, with a particular focus on the earliest possible electromagnetic radiation from the merger, the precursor light produced as the neutron stars spiral toward each other before the main event. The researchers will perform simulations of the interacting magnetic fields of merging neutron stars, estimating the power, angular pattern and broadband emission mechanisms, from possible coherent radio waves to X-rays. The project combines research in broad areas of high energy astrophysics and plasma physics. The project addresses diverse problems in multi-messenger astrophysics related to gravitational wave astronomy, interaction of ultra-strong magnetic fields and acceleration of sub-atomic particles. The results of the investigation will also help formulate the strategies for searching for possible merger precursor emission. The research will include involvement of undergraduate students at both universities and an outreach program including animated movies of the interactions being studied.The most likely scenario to generate precursor emission is the electromagnetic interaction of two neutron stars via the creation of inductive electric fields through the relative motion of magnetized plasma within the common neutron star magnetosphere. It is expected that merger times, at least millions of years after the formation of the second neutron star, are sufficiently long that, at the time of the merger, each magnetosphere is likely to be dead on its own. As the stars spiral in, the magnetospheres can be revived due to the relative orbital motion. The main goal of the project is to study this orbital revival of the common magnetospheres by employing the pulsar magnetosphere paradigm: the generation of the inductive electric field due to the motion of magnetized plasma and ensuing vacuum breakdown. The researchers will consider the formation of gaps: regions with high electric field along magnetic field lines, and reconnection layers in the orbital-modulated common magnetosphere of interacting neutron stars. Spins and orbital motion of the neutron stars may generate conditions favorable for dynamo action within the common magnetosphere, which will amplify the magnetic field. The team will also study the generation of high brightness coherent radio emission via the production of a plasma maser. This project advances the goals of the NSF Windows on the Universe Big Idea.This award reflects NSF's statutory mission and has been deemed worthy of support through evaluation using the Foundation's intellectual merit and broader impacts review criteria.

2017年8月，从两位中子星的合并中检测引力波是天体物理学的一个开创性事件。这两个非常密集的前恒星的融合与短伽马射线爆发（GRB）有关，这清楚地表明，合并提供了这种非常明亮的天体物理爆炸类型的短期类别的中心发动机。为了更好地了解中子星的合并如何产生短期GRB，普渡大学和普林斯顿大学之间的研究合作将对合并进行理论和数值研究，特别关注合并最早可能的电磁辐射，这是最早的电磁辐射，即先前的恒星在对彼此的互动中产生的前一个恒星在主赛事前都旋转。研究人员将对合并中子星的相互作用磁场进行模拟，从而估算从可能的相干无线电波到X射线的功率，角模式和宽带发射机制。该项目结合了高能量天体物理学和血浆物理学的广泛领域的研究。该项目解决了与重力波天文学有关的多通子天体物理学的各种问题，超高磁场的相互作用以及亚原子颗粒的加速度。调查的结果还将有助于制定寻找可能合并前体排放的策略。这项研究将包括大学的大学生和外展计划的参与，包括动画电影的互动电影。最有可能产生前体发射的情况是通过在普通中子中子中磁化的相对运动的相对运动来产生两个中子星的电磁相互作用，这是两个中子星的电磁相互作用。预计第二个中子恒星形成后至少数百万年的合并时间足够长，因此在合并时，每个磁层可能会自行死亡。随着恒星的螺旋，由于相对轨道运动，磁层可以恢复。该项目的主要目的是通过采用脉冲星磁层范式来研究这种轨道的轨道复兴：由于磁化等离子体的运动和随之而来的真空击穿，导致电气场的产生。研究人员将考虑差距的形成：沿磁场线高电场的区域，以及相互作用中子恒星的轨道调节的常见磁层中的重新连接层。中子星的旋转和轨道运动可能会产生有利于在常见磁层内发电机作用的条件，这将扩大磁场。该团队还将通过生产等离子Maser来研究高亮度相干的无线电排放。该项目促进了NSF Windows在宇宙大想法上的目标。该奖项反映了NSF的法定任务，并且使用基金会的知识分子优点和更广泛的影响审查标准，被认为值得通过评估来获得支持。