Modelling an X-class solar are combining observations, electron beam transport physics and MHD numerical simulations

X 级太阳能建模结合了观测、电子束传输物理和 MHD 数值模拟

• 批准号: 2597957
• 金额: --
• 依托单位: Northumbria University
• 依托单位国家: 英国
• 项目类别: Studentship
• 财政年份: 2020
• 资助国家: 英国
• 起止时间: 2020 至 无数据
• 项目状态: 未结题
• 来源: https://gtr.ukri.org/projects?ref=studentship-2597957
• 关键词: Modelling; class; solar; combining; observations

Background Information: Solar flares are sudden and large explosions of energy caused by the reconnection of magnetic field lines on the Sun's surface. The energy released spans the full range of the electromagnetic spectrum. X-class flares are the most powerful class of solar flare, and this research proposal will explore one of the most unique observations ever taken of an X-class flare, lasting for 1 hour on 10-June-2014, offering bespoke images and spectral diagnostics at incredible spatial and temporal resolution. The flare ribbons imaged are intensely bright, signifyingthe collision of powerful electron beams that traverse from the relatively low plasma density solar corona into the relatively high-density chromosphere below, leading to Bremsstrahlung radiation. The chromosphere responds to this beam injection by rapidly heating and expanding into post-flare magnetic arcades filling the loops with high-speed counter-flowing dense plasma, giving rise to a wide range of plasma fluid instabilities. We can constrain the physical processes in solar flares by diagnosing and forward modeling the highly-resolved spectral observations, assimilating them into numerical models of plasma flows, and deriving electron beam properties.Aims and Objectives: In this project, we will use a unique observation at the highest resolution of a rarely observed X-class mentioned previously to improve our comprehension of plasma physics processes in solar flares. The project will work in two stages. The first stage will involve a detailed exploration of the rapidly evolving large-scale flare phenomenon using coordinated space and ground-based multi-instrument observations spanning a wide range of absorption and emission spectral lines in the near-IR, visible, (E)UV, and X-ray wavelength channels. The insightsgained from this data analysis will allow us to develop sophisticated models of the electron beam transport leading to the flare ribbon formation, as well as to initialize advanced 3D MHD simulations of the chromospheric response to the flare ribbon formation.1 Exploration of are ribbon formation and evolution: The researcher will learn image processing techniques and explore the Swedish 1-m Solar Telescope (SST) and Solar Dynamics Observatory (SDO) image and spectral observations of the are ribbon formation, utilizing 3D visualization software. These will be used to characterize the flare ribbons' statistical properties and dynamic behaviour.2 Electron beam transport modelling incorporating observations of X-ray signatures during the flare-X-ray signatures from RHESSI observations of the flare that capture emissions near the source of the electron beam acceleration site will be forward-modelled using object-based spectroscopy software. This will allow us to examine the electron flux properties near the loop tops in the corona and during ribbon formation in the chromosphere. The results derived from objective one shall be used to model the transport and energy deposition of electrons. 3 3D MHD modelling of post-flare loop formation: Using the observationally derived properties from Objective one and two, the researcher will develop advanced 3D MHD models of plasma flows and instabilities in curved loop simulations using the numerical code Lare3D. We shall be modeling the plasma processes in a solar loop in the form of a half-torus and presenting the data in the format of an observing platform(forward modelling).

背景资料：太阳耀斑是由太阳表面磁力线重连引起的突然的能量大爆炸。释放的能量跨越电磁波谱的整个范围。X级耀斑是太阳耀斑中最强大的一类，这项研究计划将探索有史以来对X级耀斑进行的最独特的观测之一，于2014年6月10日持续1小时，以令人难以置信的空间和时间分辨率提供定制图像和光谱诊断。所拍摄到的耀斑带非常明亮，这意味着强大的电子束从相对较低的等离子体密度的日冕进入相对较高密度的色球层，导致韧致辐射。色球层对这种光束注入的反应是迅速加热并膨胀成耀斑后的磁弧，用高速逆流的致密等离子体填充环，从而引起广泛的等离子体流体不稳定性。我们可以通过诊断和正演模拟的高分辨率光谱观测，同化到等离子体流的数值模型，并推导出电子束properties.Aims和Objectives：在这个项目中，我们将使用一个独特的观察在最高分辨率的一个很少观察到的X级前面提到的，以提高我们的理解等离子体物理过程中的太阳耀斑的物理过程。该项目将分两个阶段进行。第一阶段将利用协调的空间和地面多仪器观测，详细探索迅速演变的大规模耀斑现象，观测范围涵盖近红外、可见光、（E）紫外和X射线波长通道的各种吸收和发射谱线。从这些数据分析中获得的见解将使我们能够开发导致耀斑带形成的电子束传输的复杂模型，以及初始化色球对耀斑带形成的响应的高级3D MHD模拟。研究人员将学习图像处理技术，并探索瑞典1米太阳望远镜（SST）和太阳动力学天文台（SDO）的图像和光谱观测的是带状形成，利用3D可视化软件。2电子束输运模型将结合耀斑期间的X射线特征观测-来自RHESSI观测的耀斑X射线特征，这些观测捕获了电子束加速场源附近的发射，将使用基于物体的光谱学软件进行正演模拟。这将使我们能够检查在日冕中的环顶部附近的电子通量特性，并在色球层中的带状物形成过程中。目标一的结果应用于模拟电子的传输和能量沉积。3耀斑后环形成的三维MHD模型：利用目标一和二的观测导出特性，研究人员将使用数值代码Lare 3D开发弯曲环模拟中等离子体流和不稳定性的先进三维MHD模型。我们将以半圆环的形式模拟太阳环中的等离子体过程，并以观测平台的格式提供数据（正演模拟）。