Consolidated Grant in Solar Physics

太阳物理学综合资助

• 批准号: ST/X000990/1
• 负责人: Lyndsay Fletcher
• 金额: $ 57.7万
• 依托单位: University of Glasgow
• 依托单位国家: 英国
• 项目类别: Research Grant
• 财政年份: 2023
• 资助国家: 英国
• 起止时间: 2023 至 无数据
• 项目状态: 未结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FX000990%2F1
• 关键词: Consolidated; Grant; Solar; Physics

In this proposal we study the dynamic Sun, to measure and understand the plasmas, particles and processes in its atmosphere and the extended heliosphere that it creates. We focus on several key unsolved problems in solar physics, that are also prototypes for a wider and deeper understanding of cosmic plasmas as a whole. Our top-level questions are: How does the Sun store and release energy in its magnetised atmosphere, and what can we learn about this process by studying the radiation that is emitted, from radio to X-rays? How do high-energy radiating particles behave in solar flares and in interplanetary space? How are they accelerated, are they beamed and do they play a key role in flares and their terrestrial impact? The magnetic field is key to everything that happens in the Sun's atmosphere. Concentrated magnetic regions emerge through the Sun's surface and into its atmosphere. Here they store energy and also interact with the pre-existing magnetic field often resulting in intense bursts of radiation known as flares, acceleration of sub-atomic particles (electrons and ions), and heating to millions of degrees. These can also lead to expulsion of magnetised plasma into space which can cause damaging `space weather'. Flares have distinctive radiation signatures that are closely related to the way that energy is transmitted along the magnetic field from the corona down to the solar surface and out into the distant heliosphere, and converted into other forms as it goes. By interpreting this radiation both from the Sun's tenuous outer atmosphere - its corona - and its denser lower atmosphere - its chromosphere - we can understand what is happening in a flare. More generally, solar magnetic fields create eccentric and dynamic shapes in the solar atmosphere, for example the clouds of cool material called prominences, apparently floating (though in reality supported by magnetic forces) above the solar surface.Our programme combines observational data from space-based and ground-based telescopes with theoretical and numerical modelling to address all of these topics, and spans a wide range of technical problems, from the modeling of radiation moving through a plasma to high-energy particle acceleration; from electromagnetic waves to relativistic particle beams; from machine learning and image processing to statistical analysis of weak signals, and from mathematical `pen-and-paper' calculations to advanced numerical simulations. We will bring all these skills to bear on questions at the heart of current efforts to better understand our nearest star.

在此提案中，我们研究了动态的太阳，以测量和理解其大气中的等离子体，颗粒和过程以及其产生的扩展的地球球。我们专注于太阳能物理学中的几个关键未解决的问题，这也是对整个宇宙等离子体的更广泛和更深入了解的原型。我们的顶级问题是：太阳存储和如何在其磁性气氛中释放能量，我们可以通过研究从无线电到X射线的发射辐射来了解这一过程什么？高能辐射颗粒在太阳耀斑和行星际空间中的表现如何？它们如何加速，光束，并且在耀斑和陆地撞击中起关键作用吗？磁场是太阳大气中发生的一切的关键。浓缩的磁区域从太阳的表面出现并进入大气。在这里，它们存储能量并与现有的磁场相互作用，通常会导致辐射爆发，称为耀斑，亚原子颗粒的加速度（电子和离子），并加热至数百万度。这些也可能导致将磁化等离子体驱逐到太空中，从而导致“空间天气”受损。耀斑具有独特的辐射特征，与沿磁场从电磁场向下传输到太阳能表面并向遥远的气压层传播的方式密切相关，并随着它的发展而转化为其他形式。通过从太阳脆弱的外部气氛（其电晕）及其较密集的大气层中解释这种辐射 - 我们可以理解耀斑中正在发生的事情。更一般地，太阳能磁场在太阳大气中产生了偏心和动态的形状，例如，在太阳能表面上方的浮出水面云称为突出的云，显然是在太阳能表面上方漂浮（尽管实际上是由磁力支撑的）。您的程序结合了从空间和地面望远镜与这些范围的广泛范围的范围的范围内的范围内的范围，从而使观察性数据结合在一起高能颗粒加速度；从电磁波到相对论粒子梁；从机器学习和图像处理到弱信号的统计分析，从数学“笔和纸”计算到高级数值模拟。我们将把所有这些技能带到目前努力的核心，以更好地了解我们最近的恒星。

项目成果

Enhanced Three-minute Oscillation above a Sunspot during a Solar Flare

• DOI: 10.3847/1538-4357/ad10a9
• 发表时间: 2023-11
• 期刊: The Astrophysical Journal
• 作者: Ya Wang;Lyndsay Fletcher;Sargam M. Mulay;Haisheng Ji;Wenda Cao

Behaviour of molecular hydrogen emission in three solar flares

三个太阳耀斑中氢分子发射的行为

• DOI: 10.1093/mnras/stad2853
• 发表时间: 2023
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: Mulay S

Requirements for Progress in Understanding Solar Flare Energy Transport: The Impulsive Phase

了解太阳耀斑能量传输的进展要求：冲动阶段

• DOI: 10.3847/25c2cfeb.701e4c96
• 发表时间: 2023
• 期刊: Bulletin of the AAS
• 作者: Kerr G

Intensity and velocity oscillations in a flaring active region

耀斑活动区域的强度和速度振荡

• DOI: 10.1093/mnras/stad3386
• 发表时间: 2024
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: Millar D

The Solar Particle Acceleration Radiation and Kinetics (SPARK) Mission Concept

• DOI: 10.3390/aerospace10121034
• 发表时间: 2023-12
• 期刊: Aerospace
• 影响因子: 2.6
• 作者: H. Reid;Sophie Musset;D. Ryan;V. Andretta;F. Auchère;Deborah Baker;F. Benvenuto;Philippa Browning;É. Buchlin;Ariadna Calcines Rosario;Steven Christe;Alain Jody Corso;J. Dahlin;Silvia Dalla;G. del Zanna;C. Denker;J. Dudík;R. Erdélyi;I. Ermolli;Lyndsay Fletcher;A. Fludra;Lucie M. Green;M. Gordovskyy;S. Guglielmino;I. Hannah;Richard Harrison;Laura A. Hayes;Andrew R. Inglis;N. Jeffrey;J. Kašparová;Graham S. Kerr;C. Kintziger;E. P. Kontar;S. Krucker;Timo Laitinen;P. Laurent;O. Limousin;David M. Long;S. Maloney;P. Massa;A. Massone;Sarah A. Matthews;Tomasz Mrozek;Valery M. Nakariakov;S. Parenti;Michele Piana;Vanessa Polito;M. Pesce-Rollins;P. Romano;A. Rouillard;Clementina Sasso;Albert Y. Shih;M. Stȩślicki;D. Orozco Suárez;L. Teriaca;Meetu Verma;Astrid M. Veronig;N. Vilmer;C. Vocks;A. Warmuth