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 月检测到两颗中子星合并产生的引力波是天体物理学的重大事件。两颗极其致密的前恒星的合并与短伽马射线爆发（GRB）有关，这清楚地表明，合并为这种异常明亮的天体物理爆炸类型的短期类提供了中心引擎。为了更好地了解中子星合并如何产生短伽玛暴，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，特别关注合并中最早可能的电磁辐射，在主要事件发生之前，中子星相互螺旋运动时产生的前兆光。研究人员将对合并中子星的相互作用磁场进行模拟，估计从可能的相干无线电波到 X 射线的功率、角度模式和宽带发射机制。该项目结合了高能天体物理学和等离子体物理学等广泛领域的研究。该项目解决了与引力波天文学、超强磁场相互作用和亚原子粒子加速相关的多信使天体物理学中的各种问题。调查结果还将有助于制定寻找可能的合并前体排放的策略。该研究将包括两所大学本科生的参与以及一项外展计划，其中包括正在研究的相互作用的动画电影。最有可能产生前体发射的场景是两颗中子星的电磁相互作用，通过相对中子星产生感应电场。共同中子星磁层内磁化等离子体的运动。预计合并时间（在第二个中子星形成后至少数百万年）足够长，以至于在合并时，每个磁层很可能自行死亡。当恒星螺旋进入时，磁层可以由于相对轨道运动而恢复。该项目的主要目标是通过采用脉冲星磁层范例来研究常见磁层的轨道复兴：由于磁化等离子体的运动和随后的真空击穿而产生感应电场。研究人员将考虑间隙的形成：沿磁场线具有高电场的区域，以及相互作用中子星的轨道调制共同磁层中的重连接层。中子星的自旋和轨道运动可能会产生有利于共同磁层内发电机作用的条件，这将放大磁场。该团队还将研究通过生产等离子体脉泽来产生高亮度相干无线电发射。该项目推进了 NSF 宇宙之窗大创意的目标。该奖项反映了 NSF 的法定使命，并通过使用基金会的智力价值和更广泛的影响审查标准进行评估，被认为值得支持。