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

背景资料：太阳耀斑是由太阳表面磁力线重连引起的突然而巨大的能量爆炸。释放的能量跨越了电磁波谱的整个范围。x级耀斑是最强大的太阳耀斑，这项研究计划将探索迄今为止对x级耀斑进行的最独特的观测之一，该观测于2014年6月10日持续了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。图像上的耀斑带非常明亮，表明强大的电子束从相对低等离子体密度的太阳日冕穿过相对高密度的色球层，导致轫致辐射的碰撞。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拱廊，使环路充满高速反向流动的致密等离子体，从而产生大范围的等离子体流体不稳定性。我们可以通过诊断和正演模拟高分辨率的光谱观测，将它们同化到等离子体流的数值模型中，并推导出电子束的性质，从而约束太阳耀斑的物理过程。目的和目标：在这个项目中，我们将使用之前提到的罕见的x级最高分辨率的独特观测来提高我们对太阳耀斑等离子体物理过程的理解。该项目将分两个阶段进行。第一阶段将包括对快速演变的大规模耀斑现象的详细探索，使用协调的空间和地面多仪器观测，跨越近红外、可见光、(E)UV和x射线波长通道的广泛吸收和发射光谱线。从该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，以及初始化对耀斑带形成的色球响应的高级3D MHD模拟探索太阳带的形成和演化：研究人员将学习图像处理技术，并利用3D可视化软件探索瑞典1米太阳望远镜（SST）和太阳动力学观测站（SDO）的图像和光谱观测。这些将用于表征耀斑带的统计特性和动态行为电子束输运建模结合了耀斑期间x射线特征的观测-来自RHESSI对耀斑观测的x射线特征，捕获了电子束加速点源附近的辐射，将使用基于对象的光谱软件进行前向建模。这将使我们能够检查日冕环顶附近和色球层带状形成期间的电子通量特性。结果来源于目标1应使用，以模拟电子的输运和能量沉积。3 .耀斑后环形成的三维MHD模型：利用目标1和目标2的观测性质，研究人员将使用数值代码Lare3D开发先进的等离子体流动和弯曲环模拟不稳定性的三维MHD模型。我们将以半圆环的形式对太阳环内的等离子体过程进行建模，并以观测平台的格式呈现数据（正演建模）。

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).