Relativistic Asymmetric Magnetic Reconnection: Theory and Kinetic Modeling

相对论不对称磁重联：理论和动力学建模

• 批准号: 2205991
• 负责人: Colby Haggerty
• 金额: $ 41.31万
• 依托单位: University of Hawaii
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2022
• 资助国家: 美国
• 起止时间: 2022-06-01 至 2025-05-31
• 项目状态: 未结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=2205991&HistoricalAwards=false
• 关键词: Relativistic; Asymmetric; Magnetic; Reconnection; Theory

This project will explore the process of magnetic reconnection in magnetized astrophysical plasmas. Most space and astrophysical systems, including the sun and stars in and out of the milky way, are made up of hot, ionized gas -- a plasma permeated by magnetic fields. Frequently, high energy light and particles are rapidly generated by these systems through a process known as magnetic reconnection. An improved understanding of magnetic reconnection and the radiation it generates will be developed by this project using computer simulations and by including more realistic conditions motivated by astrophysical observations. The simulations will be used to connect the conditions of the plasma to the characteristics of the radiation. The research effort will improve our understanding of how astrophysical plasmas behave and what are the sources of high energy radiation from our galaxy and beyond. This project is jointly funded by the Division of Physics, the Division of Astronomical Sciences, and the Established Program to Stimulate Competitive Research (EPSCoR).The fundamental plasma process of magnetic reconnection will be studied in the relativistic and asymmetric limit, in regimes where the magnetic energy per particle is larger than the rest mass energy and the plasma properties of the interacting magnetic structures differ from each other. The project will attempt to achieve three key goals: (1) develop scaling predictions for relativistic, asymmetric magnetic reconnection; (2) identify relationships between the initial asymmetric plasma parameters and the energetic, non-thermal particle distributions generated by reconnection; and (3) explore the contribution of magnetic reconnection to the non-thermal particle distribution in a global astrophysical system. The first two goals will be approached by performing a survey of plasma simulations of magnetic reconnection, which will be analyzed and compared with derived theoretical predictions. The third goal will be achieved by examining relativistic jet simulations of active galactic nuclei to estimate the reconnection-generated non-thermal spectrum of energetic particles. The parameter regimes to be explored, along with the application to relativistic jets is directly relevant to the growing field of plasma astrophysics and can provide insight into the origin of accelerated high energy particles and the associated impulsive emission in astrophysics.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.

该项目将探索磁化天体物理等离子体中磁重联的过程。 大多数空间和天体物理系统，包括太阳和银河系内外的恒星，都是由热的电离气体——一种充满磁场的等离子体组成。通常，这些系统通过称为磁重联的过程快速产生高能光和粒子。该项目将使用计算机模拟并纳入由天体物理观测激发的更现实的条件，从而更好地理解磁重联及其产生的辐射。模拟将用于将等离子体的条件与辐射的特性联系起来。这项研究工作将增进我们对天体物理等离子体行为方式以及银河系及其他地区高能辐射来源的理解。 该项目由物理系、天文科学系和刺激竞争性研究既定计划（EPSCoR）联合资助。磁重联的基本等离子体过程将在相对论和不对称极限下进行研究，其中每个粒子的磁能大于其余质量能，并且相互作用的磁结构的等离子体特性彼此不同。该项目将尝试实现三个关键目标：（1）开发相对论性、不对称磁重联的尺度预测； (2) 确定初始不对称等离子体参数与重联产生的高能、非热粒子分布之间的关系； (3)探索磁重联对全球天体物理系统中非热粒子分布的贡献。前两个目标将通过对磁重联的等离子体模拟进行调查来实现，并对磁重联的等离子体模拟进行分析并与导出的理论预测进行比较。第三个目标将通过检查活动星系核的相对论喷流模拟来估计重联产生的高能粒子非热谱来实现。待探索的参数体系以及相对论射流的应用与不断发展的等离子体天体物理学领域直接相关，并且可以深入了解加速高能粒子的起源以及天体物理学中相关的脉冲发射。该奖项反映了 NSF 的法定使命通过使用基金会的智力优点和更广泛的影响审查标准进行评估，并被认为值得支持。

项目成果

Relativistic Asymmetric Magnetic Reconnection

相对论不对称磁重联

• DOI: 10.1103/physrevlett.128.145101
• 发表时间: 2022-04
• 期刊: Physical Review Letters
• 影响因子: 8.6
• 作者: Mbarek, Rostom;Haggerty, Colby;Sironi, Lorenzo;Shay, Michael;Caprioli, Damiano
• 通讯作者: Caprioli, Damiano