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Photospheric Flare Diagnositics

光球耀斑诊断

基本信息

批准号：
2302544
负责人：
金额：
--
依托单位：
Queen's University Belfast
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-2302544
关键词：
Photospheric Flare Diagnositics

项目摘要

The prevailing model for flare initiation is based on an electron beam that penetrates the lower atmosphere, producing explosive evaporation and heating to high temperatures. Despite numerous studies of evaporation processes in the chromosphere and corona, the impact of the flare beams to the photospheric velocity profiles has remained unexplored. The project will combine state-of-the-art simulations with observations to address important questions on the impact of flares on solar/stellar atmospheres. This project's focus on the photosphere's response to a solar flare sets it apart from previous works which have focused on the more dramatic response of the chromosphere. At this much lower height in the solar atmosphere, the effects of a flare are greatly reduced, but the observational signatures of the processes at work can be identified in spectral lines and continua across the electromagnetic spectrum. It is therefore the purpose of this project to investigate through radiative-hydrodynamic (RHD) modelling if there may be observable shifts in line spectra formed in the photosphere. Such shifts, even if on the order of m/s, are important to establish when considering exoplanet detection around distant stars to avoid false attribution of line shifts that are actually due to stellar flares. The main objectives of the project are:Use the F-CHROMA grid of flare models to identify the effects of electron beams at the deepest layers of the solar atmosphere.Expand the existing grid by including protons beams and direct heating.Perform line synthesis to identify the photospheric lines that show the strongest response to the heating.Compare the simulated spectra with high resolution spectroscopic observations.Use the simulations to define the science goals of future ground-based and space-borne observatories. These observatories include the Daniel K Inouye Solar Telescope, European Solar Telescope, Solar Orbiter and others.Other information:QUB has been a member of F-CHROMA (www.fchroma.org), a research consortium funded by the European Commission, that focused on space-based and ground-based multi-mode, multi-wavelength studies of solar flares. The student will work in collaboration with an international team of researchers at QUB, Europe and the US.Facilities to be usedRADYN & RH (Radiative Hydrodynamic Codes), Swedish Solar Telescope (La Palma), Daniel K Inouye Solar Telescope (Maui)

目前流行的耀斑启动模型是基于穿透低层大气的电子束，产生爆炸性蒸发并加热至高温。尽管对色球和日冕中的蒸发过程进行了大量研究，但耀斑光束对光球层速度分布的影响仍未得到探索。该项目将把最先进的模拟与观测相结合，以解决耀斑对太阳/恒星大气影响的重要问题。这个项目的重点是光球层对太阳耀斑的反应，这与以前的工作不同，以前的工作关注的是色球更戏剧性的反应。在太阳大气的这个低得多的高度，耀斑的影响大大减少，但工作过程的观测特征可以在电磁光谱的谱线和连续体中识别出来。因此，本项目的目的是通过辐射-流体动力学(RHD)模型调查在光球层中形成的线谱是否可能有可观察到的移位。在考虑对遥远恒星周围的系外行星进行探测时，即使是m/S量级的这种移动也是重要的，以避免错误地归因于实际上是由恒星耀斑引起的线移。该项目的主要目标是：使用耀斑模型的F-Chroma网格来确定太阳大气最深处的电子束的影响。通过包括质子束和直接加热来扩展现有的网格。进行线合成以确定对加热反应最强烈的光球线。将模拟光谱与高分辨率光谱观测进行比较。使用模拟来确定未来地面和空间天文台的科学目标。这些天文台包括丹尼尔·K·井上太阳望远镜、欧洲太阳望远镜、太阳轨道器等。其他信息：昆士兰大学一直是F-Chroma(www.fchroma.org)的成员，F-Chroma是一个由欧盟委员会资助的研究联盟，专注于空间和地面的多模式、多波长的太阳耀斑研究。这名学生将与QUB、欧洲和美国的一个国际研究团队合作。将使用的设施包括RADYN&RH(辐射流体动力学代码)、瑞典太阳望远镜(拉帕尔马)、丹尼尔·K·井上太阳望远镜(MAUI)