Revealing the Pattern of Solar Alfvénic Waves - RiPSAW

揭示太阳阿尔弗尼波的模式 - RiPSAW

• 批准号: MR/T019891/1
• 负责人: Richard Morton
• 金额: $ 163.83万
• 依托单位: Northumbria University
• 依托单位国家: 英国
• 项目类别: Fellowship
• 财政年份: 2020
• 资助国家: 英国
• 起止时间: 2020 至 无数据
• 项目状态: 未结题
• 来源: https://gtr.ukri.org/projects?ref=MR%2FT019891%2F1
• 关键词: Revealing; Pattern; Solar; Alfv; nic

This research proposal aims to make advances in our understanding of the physics of our closest star, the Sun, and other solar-like stars. The Sun displays a number of fascinating and dynamic phenomena such as powerful solar flares and giant, planet-sized concentrations of magnetic fields (sunspots). It also provides a unique window that permits us to examine in detail how other stars behave. The Sun is made of a plasma (ionised gas) threaded by a strong magnetic field. Such magnetised plasmas are common throughout the universe (e.g. active galaxy nuclei, nebula, interstellar medium), hence the research will also aid advances across multiple research communities. Many stars possess their own weather systems, although these systems are extreme compared to those we experience on Earth. In our solar system, a hot, million degree wind blows off the Sun at colossal speeds reaching millions of miles per hour, washing over the planets. While we are under the protection of the Earth's magnetic field, that deflects the Sun's wind, other planetary bodies in the solar system have been exposed to its influence. For example, the Sun's wind is known to have stripped Mars of its atmosphere. Scientists are also interested in how these winds will influence the habitability of exoplanets around other Sun-like stars. These winds also contribute to how the stars evolve, with the Sun losing over 10 trillion tonnes of material each year via its winds. The objectives of the RiPSAW project are to examine a new mechanism related to the generation of the hot plasma and powerful winds, focusing on the role of magnetic waves. These magnetic (or Alfvén) waves are able to transfer energy through a star's atmosphere and are considered an important feature of any magnetic star. Exciting results from Dr Morton's recent observations of the Sun have found evidence that the magnetic waves are excited high in the atmosphere by sound waves leaking out from the inside of the Sun. This challenges our current knowledge of how energy is transported through a stars' atmosphere, hence the proposed work may transform the understanding of how these hot winds behave.To address these fundamental, yet unanswered, questions, RiPSAW makes use of advanced mathematical techniques and cutting-edge computer simulations to create models of the Sun based on magnetohydrodynamics. We combine this theoretical effort with the highest quality data of the Sun available from state-of-the-art solar instruments (e.g. NASA's Solar Dynamic Observatory); incorporating information from across the electromagnetic spectrum (e.g. visible, EUV) and analysing this with modern methods drawn from statistics and machine learning.

这项研究计划旨在增进我们对距离我们最近的恒星——太阳和其他类太阳恒星的物理现象的理解。太阳展现出许多令人着迷的动态现象，例如强大的太阳耀斑和行星大小的巨大浓度。它还提供了一个独特的窗口，使我们能够详细研究太阳是如何由强磁场穿过的等离子体（电离气体）组成的。宇宙（例如活跃星系原子核、星云、星际介质），因此这项研究也将有助于多个研究团体的进步，尽管这些系统与我们在太阳系中经历的天气系统相比是极端的。度风以每小时数百万英里的速度吹走太阳，冲刷着行星。当我们处于地球磁场的保护之下时，太阳风会偏转，而太阳系中的其他行星体却受到了影响。它是例如，众所周知，太阳风带走了火星的大气层，这些风将如何影响其他类太阳恒星周围的系外行星的宜居性，这些风也有助于恒星的演化。太阳每年通过风损失超过 10 万亿吨物质，RiPSAW 项目的目标是研究与热等离子体和强风产生相关的新机制，重点关注磁波的作用。或者阿尔文）波能够通过恒星的大气层传递能量，被认为是任何磁星的一个重要特征。莫顿博士最近对太阳的观测发现了令人兴奋的结果，表明磁波在大气层中是被泄漏的声波激发的。这挑战了我们目前对能量如何通过恒星大气层传输的知识，因此拟议的工作可能会改变对这些热风行为的理解。为了解决这些基本但尚未解答的问题，RiPSAW利用先进的数学技术和尖端的计算机模拟来创建基于磁流体动力学的太阳模型，我们将这一理论成果与最先进的太阳仪器（例如美国宇航局的太阳能仪器）提供的最高质量的太阳数据结合起来。动态天文台）；整合来自整个电磁频谱（例如可见光、EUV）的信息，并使用统计和机器学习中的现代方法进行分析。

项目成果

Magnetohydrodynamic Simulations of Spicular Jet Propagation Applied to Lower Solar Atmosphere Model

应用于低层太阳大气模型的针状射流传播的磁流体动力学模拟

• DOI: http://dx.10.3847/1538-4357/abefd1
• 发表时间: 2021
• 期刊: The Astrophysical Journal
• 作者: Mackenzie Dover F

An overall view of temperature oscillations in the solar chromosphere with ALMA.

使用 ALMA 全面了解太阳色球层的温度振荡。

• DOI: http://dx.10.1098/rsta.2020.0174
• 发表时间: 2021
• 期刊: Philosophical transactions. Series A, Mathematical, physical, and engineering sciences
• 作者: Jafarzadeh S

Magnetohydrodynamic Simulations of Spicular Jet Propagation Applied to Lower Solar Atmosphere Model. II. Case Studies with Tilted Jets

应用于低层太阳大气模型的针状射流传播的磁流体动力学模拟。

• DOI: 10.3847/1538-4357/ac5aa9
• 发表时间: 2022-04-01
• 期刊: The Astrophysical Journal
• 作者: Fionnlagh Mackenzie Dover;Rahul Sharma;R. Erdélyi
• 通讯作者: R. Erdélyi

The Role of High-frequency Transverse Oscillations in Coronal Heating

高频横向振荡在日冕加热中的作用

• DOI: http://dx.10.3847/2041-8213/ace423
• 发表时间: 2023
• 期刊: The Astrophysical Journal Letters
• 作者: Lim D

Weak Damping of Propagating MHD Kink Waves in the Quiescent Corona

静止电晕中传播 MHD 扭结波的弱阻尼

• DOI: 10.3847/1538-4357/ac324d
• 发表时间: 2021-05-25
• 期刊: The Astrophysical Journal
• 作者: R. Morton;A. Tiwari;T. Van Doorsselaere;J. McLaughlin
• 通讯作者: J. McLaughlin