A HIGH-RESOLUTION IMAGING SPECTROMETER FOR VISIBLE CORONAL EMISSION LINES

用于可见日冕发射线的高分辨率成像光谱仪

• 批准号: ST/N002962/1
• 负责人: Huw Morgan
• 金额: $ 30.6万
• 依托单位: Aberystwyth University
• 依托单位国家: 英国
• 项目类别: Research Grant
• 财政年份: 2016
• 资助国家: 英国
• 起止时间: 2016 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FN002962%2F1
• 关键词: RESOLUTION; IMAGING; SPECTROMETER; VISIBLE; CORONAL

The Earth orbits through a sea of magnetised plasma flowing from the Sun called the solar wind. Travelling at high speed through the solar wind, Coronal Mass Ejections (CME) are enormous clouds of high-density plasma associated with eruptions and flares at the Sun. The Earth's magnetic field acts as a shield to prevent damage from CMEs. Society, however, depends on satellites and large CMEs under certain conditions may cause widespread damage. The ability to predict the occurrence of a CME, and to predict their subsequent evolution, depends critically on understanding the dominant physical processes which occur in the corona, and on understanding the medium through which CMEs propagate - the solar wind. In understanding the solar wind and CMEs, the extended inner corona is a critical region. This complex region starts at the solar surface and extends to where the coronal plasma starts to expand radially and becomes supersonic. Current observations of this region are very limited. There are a handful of broadband visible light coronagraphs which provide rather noisy measurements of the Thomson-scattered light from coronal electrons such as the COR1/STEREO coronagraphs, or the MLSO MKIV coronameters (to be upgraded to COSMO soon). Current EUV imagers and spectrometers provide very high-quality data, but their field of view is typically limited to a few tenths of solar radii from the photosphere at best. There is no spectrometer currently in use which can observe the corona above a few tenths of a solar radius from the limb, severely restricting efforts to understand the source region of CMEs and the solar wind.The goal of the proposed spectrometer is to capitalize on the diagnostic properties of coronal forbidden emission lines in the visible and near-IR, to infer electron temperatures, ion densities, elemental abundances and charge states, bulk flow speeds, non-thermal heating (i.e. wave heating) and indirectly the properties of the coronal magnetic field. The scientific advantage of observing these lines stems primarily from the strength of their radiatively excited component, which enables the emission to extend out to large heliocentric distances. It is surprising therefore that observations of forbidden coronal emission lines in the visible have been seriously neglected in current solar missions. The proposed spectrometer directly addresses this shortcoming and will provide unique constraints on the physical processes that heat the solar atmosphere to over one million degrees and accelerate the solar wind.

地球绕地球运行，穿过来自太阳的磁化等离子体海洋，称为太阳风。日冕物质抛射 (CME) 高速穿过太阳风，是与太阳喷发和耀斑相关的巨大高密度等离子体云。地球磁场充当屏障，防止日冕物质抛射造成损害。然而，社会依赖于卫星，大型日冕物质抛射在某些条件下可能会造成广泛的损害。预测日冕物质抛射发生以及预测其随后演化的能力在很大程度上取决于对日冕中发生的主要物理过程的了解，以及对日冕物质抛射传播的介质——太阳风的了解。在了解太阳风和日冕物质抛射过程中，扩展的内日冕是一个关键区域。这个复杂的区域从太阳表面开始，延伸到日冕等离子体开始径向膨胀并变成超音速的地方。目前对该地区的观察非常有限。有一些宽带可见光日冕仪可以对来自日冕电子的汤姆逊散射光进行相当嘈杂的测量，例如 COR1/STEREO 日冕仪或 MLSO MKIV 日冕仪（即将升级到 COSMO）。目前的 EUV 成像仪和光谱仪可提供非常高质量的数据，但它们的视野通常最多仅限于距光球层太阳半径的十分之几。目前使用的光谱仪还没有能够观测距边缘几十分之几太阳半径以上的日冕，这严重限制了了解日冕物质抛射源区和太阳风的努力。所提出的光谱仪的目标是利用可见光和近红外日冕禁发射线的诊断特性，推断电子温度、离子密度、元素丰度和电荷状态、体积 流速、非热加热（即波加热）和间接日冕磁场的特性。观察这些线的科学优势主要源于其辐射激发成分的强度，这使得发射能够延伸到较大的日心距离。因此，令人惊讶的是，在当前的太阳任务中，对可见光中禁止的日冕发射线的观测被严重忽视。所提出的光谱仪直接解决了这一缺点，并将对将太阳大气加热到超过一百万度并加速太阳风的物理过程提供独特的限制。

项目成果

Derived Electron Densities from Linear Polarization Observations of the Visible-Light Corona During the 14 December 2020 Total Solar Eclipse

• DOI: 10.1007/s11207-023-02231-5
• 发表时间: 2023-10
• 期刊: Solar Physics
• 影响因子: 2.8
• 作者: Liam T. Edwards;Kaine A. Bunting;Brad Ramsey;Matt Gunn;Tomos Fearn;Thomas Knight;Gabriel D. Muro;Huw Morgan

Dynamics of Large-scale Coronal Structures as Imaged during the 2012 and 2013 Total Solar Eclipses

2012 年和 2013 年日全食期间成像的大型日冕结构的动力学

• DOI: 10.3847/1538-4357/aa8cd2
• 发表时间: 2017
• 期刊: The Astrophysical Journal
• 作者: Alzate N

Low-Coronal Sources of Stealth CMEs

隐形日冕物质抛射的低日冕源

• 发表时间: 2016
• 期刊: AAS/Solar Physics Division Abstracts #47
• 作者: Alzate Nathalia

JETS, CORONAL "PUFFS," AND A SLOW CORONAL MASS EJECTION CAUSED BY AN OPPOSITE-POLARITY REGION WITHIN AN ACTIVE REGION FOOTPOINT

• DOI: 10.3847/0004-637x/823/2/129
• 发表时间: 2016-06-01
• 期刊: ASTROPHYSICAL JOURNAL
• 影响因子: 4.9
• 作者: Alzate, N.;Morgan, H.
• 通讯作者: Morgan, H.

Identification of Low Coronal Sources of "Stealth" Coronal Mass Ejections Using New Image Processing Techniques

• DOI: 10.3847/1538-4357/aa6caa
• 发表时间: 2017-05-10
• 期刊: ASTROPHYSICAL JOURNAL
• 影响因子: 4.9
• 作者: Alzate, Nathalia;Morgan, Huw
• 通讯作者: Morgan, Huw