The Dynamics of Thin Current Sheets and the Triggering of Fast Reconnection in Different Plasma Environments

这项研究旨在了解可见宇宙中一些最具能量的事件和美丽光芒的触发机制。空间和天体物理等离子体--构成可见(重子)宇宙最大部分的电离气体--是各种观测到的能量现象的原因，从脉冲星伽马射线耀斑到太阳耀斑，再到导致北极光的磁层亚暴。所有这些过程的特征都是能量存储的初步阶段，在这个阶段，磁场能量由于等离子体的旋转、重力或对流运动而建立，随后突然触发快速能量释放。磁重联，即磁力线的拼接和重塑，被认为是大多数观察到的爆炸现象的核心。这项研究的结果将使人们能够更好地理解从稳定到突然释放磁能的转变，并能够预测不同天体物理以及实验室等离子体中发生转变所需的关键参数。S这个研究项目的更广泛影响包括在实验室和天体物理背景下对这个数十年前的等离子体物理问题的更高级理解，应用涉及未来的实验室实验和高级数值计算，以及美国宇航局的任务。磁重联的经典图像涉及电流片，假设为平面状，非常狭窄地集中在第三维空间。最近，由于发现这种构型不稳定到撕裂较大的伦德奎斯特数S，改变了缓慢、稳定的重连情景，导致了一幅有希望的图景(又名。等离子体不稳定)的快速重新连接。平面电流片的等离子体不稳定具有一个悖论特征，即不稳定增长率与S增长率发散，S增长率在较高时变得任意大。S因此提出了系统如何从稳定向不稳定转变的问题。Pucci和Velli最近解决了增长率差异带来的这个难题，他们指出，限制电流片的逆长宽比将慢速和快速重新连接模式分开，他们将这种特性称为“理想撕裂”，或IT。其结果是，在相对较厚的电流片和所有等离子体不稳定标度(岛数等)中出现快速重联。需要更正。这样的场景是有希望的，因为它不仅可以解释观察到的快速重新连接速率，而且还可以解释重新连接触发机制。本研究计划建立在IT重联框架的基础上，并将其推广到不同区域的不同等离子体构型：1)将线性标度理论扩展到更一般的平衡和包括流动和动力学区域在内的二维；2)模拟3D阻性磁流体中的崩塌电流片，以研究有和没有初始流动时构型的非线性演化。这一结果将影响对自然和实验室等离子体中灾难性能量释放的理解。

This research aims to understand the triggering mechanism for some of the most energetic events and beautiful light shows in the visible universe. Space and astrophysical plasmas - the ionized gases constituting the greatest part of the visible (baryonic) Universe - are responsible for a variety of observed energetic phenomena from pulsar gamma-ray flares, to solar flares, to magnetospheric substorms leading to Aurora Borealis. All of these processes are characterized by a preliminary phase of energy storage, where magnetic field energy is built up due to rotational, gravitational, or convective motions of the plasma, followed by the sudden triggering of rapid energy release. Magnetic reconnection, the splicing and reforming of magnetic field lines is thought to be at the heart of most observed explosive phenomena. The results of this research will allow a better understanding of the transition from stability to the sudden release of magnetic energy, with the ability to predict the critical parameters necessary for the transition in different astrophysical, as well as laboratory plasmas. This research project?s broader impact includes a more advanced understanding of this decades-old plasma physics problem both in laboratory and astrophysical contexts, with applications involving future laboratory experiments and advanced numerical computations, as well as NASA missions.The classic picture of magnetic reconnection involves current sheets, assumed to be planar-like and concentrated very narrowly in the third dimension. Recently, the slow, stationary reconnection scenario was transformed by the discovery that such configuration is unstable to tearing at large values of the Lundquist number, S, leading to one promising picture (a.k.a. the plasmoid instability) of fast reconnection. The plasmoid instability of the planar current sheet has a paradoxical feature, in that the instability growth rate diverges with S. Growth rates which become arbitrarily large at high S therefore beg the question of how a system transitions from stability to instability. This difficulty with diverging growth rates was resolved recently by Pucci and Velli, who showed that a limiting current sheet inverse aspect ratio separates slow and fast reconnecting modes, a property they called "Ideal Tearing", or IT. As a consequence, fast reconnection sets in in relatively thick current sheets and all plasmoid instability scalings (number of islands etc.) require correction. Such a scenario is promising in that it not only can explain observed fast reconnection rates, but might also account for the reconnection trigger mechanism. The present research program builds on the IT reconnection framework and generalizes it to different plasma configurations in different regimes by: 1) extending the linear scaling theory to more general equilibria and two dimensions including flows and kinetic regimes; 2) simulating collapsing current sheet in 3D resistive MHD to study nonlinear evolution in configurations with and without initial flows. The results will impact the understanding of catastrophic energy release in natural and laboratory plasmas.