Integrated Mapping of Temperature, Density, Iron Abundance and Magnetic Field Structure in the Inner Corona During Total Solar Eclipses

研究人员将试图区分快慢太阳风的起源。主要工作是研究即将到来的两次日全食时日冕的几个特性。研究人员将同时进行k -日冕，Fe X， XI， XIII和XIV强度成像，Fe XIV的光谱成像和Fe XIII和XIV的偏振成像。从这些数据中，他们将推断出电子密度、温度、视线速度、Fe+12和Fe+13离子的丰度，以及磁场方向的“天平面”投影。人们普遍认为，慢风来自磁场封闭的日冕区域，而快风来自磁场开放的区域，但这是一种分类，而不是一种理解。物理理解只能来自对不同源区的等离子体参数的了解。研究人员指出，目前观测技术之间的差异阻碍了对这些参数的明确确定。他们对电子密度和温度的新测量代表了解决这些差异的尝试。

The investigators will attempt to distinguish the origins of fast and slow solar wind. The main effort is to study several properties of the solar corona at two forthcoming total solar eclipses. The investigators will make simultaneous K-corona, Fe X, XI, XIII and XIV intensity imagery, spectroscopic imaging in Fe XIV, and polarimetric imaging in Fe XIII and XIV. From these, they will deduce electron density, temperature, line-of-sight velocity, abundance of Fe+12 and Fe+13 ions, and the "sky plane" projection of the magnetic field direction. It is widely accepted that slow wind comes from areas of the corona with closed magnetic fields, and fast wind from regions with open magnetic fields, but this is a classification rather than an understanding. Physical understanding can only come from knowledge of the plasma parameters in the different source regions. The investigators note that discrepancies among current observational techniques currently prevent unambiguous determination of these parameters. Their new measurements of electron density and temperature represent an attempt to resolve these discrepancies.