Understanding CMEs using AIA and SWAP data

太阳是一颗充满活力的活跃的星星。从伽马射线到无线电的整个电磁频谱的观测表明，太阳有一百万度的大气层，太阳系中最具能量的爆炸和爆发发生在其中。爆炸被称为太阳耀斑，爆发被称为日冕物质抛射（CME）。这些高能现象的能量来源是太阳大气磁场中的场向电流。了解将这种能量从磁场转换为其他形式（如动能和辐射）的物理过程，从而了解耀斑和CME，是太阳物理学的一个主要目标。该项目的目的是研究导致日冕物质抛射的物理现象的演变，在许多情况下，一个关键方面是磁场形成日冕物质抛射是一种被称为“通量绳”的配置。这些是扭曲的磁场束，它们可能会失去稳定性，然后爆发到太阳系中。然而，观测结果表明，爆发的磁结构可能不是最初形成的整个磁绳，这就提出了一个问题，即在CME之前不久，发生了什么物理过程来演变这种配置。该项目旨在了解通量绳是如何形成的，以及由于周围日冕磁场的影响而在喷发之前和期间发生的变化。该项目将使用SDO和Proba-2航天器以及地面望远镜提供的一系列数据集。

The Sun is a dynamic and active star. Observations across the electromagnetic spectrum from gamma rays to radio have revealed that the Sun has a million degree atmosphere in which the most energetic explosions and eruptions in the Solar System take place. The explosions are known as solar flares and the eruptions are known as coronal mass ejections (CMEs). The energy source for these energetic phenomena is field-aligned electric currents in the Sun's atmospheric magnetic field. Understanding the physical processes that take place to convert this energy from magnetic to other forms such as kinetic and radiative and hence understand flares and CMEs, is a major aim in solar physics. The aim of this project is to study the evolution of the physical phenomena leading to the initiation of CMEs.In many cases, a key aspect is that the magnetic field forms a CME is a configuration known as a "flux rope". These are bundles of twisted magnetic field, which can lose their stability and then erupt into the Solar System. However, observations indicate that the magnetic structure that erupts might not be the entire flux rope as initially formed, raising the question of what physical processes are occurring to evolve the configuration shortly before the CME. This project seeks to understand how flux ropes form and are modified before and during the eruption itself due to the influence of the surrounding coronal magnetic field. The project will use a range of data sets supplied by the SDO and Proba-2 spacecraft, as well as ground-based telescopes.