Understanding how elemental abundances vary with time in the solar atmosphere

了解太阳大气中元素丰度如何随时间变化

• 批准号: 2238160
• 金额: --
• 依托单位: University College London
• 依托单位国家: 英国
• 项目类别: Studentship
• 财政年份: 2019
• 资助国家: 英国
• 起止时间: 2019 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=studentship-2238160
• 关键词: Understanding; how; elemental; abundances; vary

Elemental abundance patterns are tracers of physical processes throughout the universe, with the cosmic reference standard being the solar chemical composition. Understanding how the Sun's chemical composition varies in time and space provides insight into how mass and energy flow through the Sun's atmosphere into the solar wind, and in turn, through the atmospheres of solar-like stars into stellar winds. The Sun mainly consists of hydrogen and helium, with trace amounts of heavier elements. Although its atmosphere (corona) should have the same elemental abundances as the surface (photosphere), easily ionized elements are enhanced by a factor 2-4 in the corona compared to their photospheric abundances; behavior known as the first ionisation potential (FIP) effect. Recent spectroscopic observations of the Sun have shown that the spatial and temporal variability of coronal composition is intrinsically linked to the evolution of the solar magnetic field. How variations in the coronal composition relate to changes in the magnetic field provides clues to the origin of solar activity (flares, jets) and the solar wind. One of the primary goals of the upcoming Solar Orbiter mission (due to launch in 2020) will be to establish the origin of the solar wind using these plasma properties.The aim of this project is to exploit the more than 12 years of spectroscopic observations of the solar corona from the joint UK-NASA-JAXA (Japanese Aerospace Exploration Agency) Extreme-ultraviolet Imaging Spectrometer (EIS) instrument onboard the Hinode ("Sunrise" in Japanese) spacecraft. This unprecedented, yet underutilised, archive provides a unique opportunity to conduct the first statisticallysignificant study of the physical processes which govern variation in composition and elemental abundance across a range of spatial and temporal scales. The project will involve learning spectroscopic analysis techniques, analysing "big data" from a large archive, proposing and obtaining new observations with Hinode/EIS in Japan and combining the spectral data with imaging and magnetic field data using state-of-the-art techniques. This will provide an opportunity to advance scientific understanding and techniques in preparation for the launch of Solar Orbiter, an ESA-led mission with strong involvement from UCL/MSSL and the Solar-C mission currently being proposed to JAXA. The project will also involve close collaboration with international experts from Japan and the USA.

元素丰度模式是整个宇宙中物理过程的示踪剂，宇宙参考标准是太阳能化学成分。了解太阳的化学成分在时间和空间上如何变化，可以洞悉质量和能量如何通过太阳的大气流入太阳风，然后通过太阳能恒星的大气进入恒星风。太阳主要由氢和氦气组成，带有痕量的较重元素。尽管它的大气（电晕）应具有与表面（Photoshere）相同的元素丰度，但与它们的光球丰度相比，Corona中的一个因子2-4易于使电离元素增强。行为称为第一个电离势（FIP）效应。最近对太阳的光谱观察结果表明，冠状成分的空间和时间变异性与太阳磁场的演化本质上联系在一起。冠状成分的变化与磁场的变化有关，为太阳能活动（耀斑，喷气机）和太阳风的起源提供了线索。 One of the primary goals of the upcoming Solar Orbiter mission (due to launch in 2020) will be to establish the origin of the solar wind using these plasma properties.The aim of this project is to exploit the more than 12 years of spectroscopic observations of the solar corona from the joint UK-NASA-JAXA (Japanese Aerospace Exploration Agency) Extreme-ultraviolet Imaging Spectrometer (EIS) instrument onboard the Hinode （日语中的“日出”）航天器。这个前所未有但未被充分利用的档案提供了一个独特的机会，可以对负责在一系列空间和时间尺度上进行组成和元素丰度变化的物理过程进行首次统计学意义研究。该项目将涉及学习光谱分析技术，分析大型档案馆的“大数据”，提出并在日本使用Hinode/eis获得新的观察结果，并使用最先进的技术将光谱数据与成像和磁场数据相结合。这将提供一个机会，以提高科学理解和技术，为推出太阳能轨道机，ESA领导的任务，并与UCL/MSSL的强烈参与以及目前正在向Jaxa提议的太阳能传教团进行了强烈参与。该项目还将与日本和美国的国际专家进行密切合作。