Fundamental plasma physics of the sun and heliosphere: Warwick CFSA Consolidated Grant Application

太阳和日光层的基础等离子体物理学：Warwick CFSA 综合拨款申请

• 批准号: ST/T000252/1
• 负责人: Sandra Chapman
• 金额: $ 105.42万
• 依托单位: University of Warwick
• 依托单位国家: 英国
• 项目类别: Research Grant
• 财政年份: 2020
• 资助国家: 英国
• 起止时间: 2020 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FT000252%2F1
• 关键词: Fundamental; plasma; physics; sun; heliosphere

Quantitative understanding of the fundamental physical processes acting in the Sun's corona and solar wind is essential not only to the physics of the Sun and its connection to the Earth's environment, but it also enhances our knowledge of astrophysical plasma processes in general. Coronal MHD waves are of direct relevance to much of the dynamics such as solar flares and eruptions and carry unique information about the plasma parameters and physical processes operating in it; coronal waves are capable of transferring energy and mechanical momentum from the convection zone into the corona and heliosphere and are associated with the development of plasma instabilities. The plasma flowing out from the sun generates a solar wind. The texture and dynamics of the solar wind is intimately connected to that of the solar corona and this highly variable plasma flow can lead to local heating which in turn accelerates the solar wind. The solar wind is accelerated to such an extent that it is in principle a turbulence laboratory so that quantifying its fluctuations has direct implications for our understanding of turbulence. Solar wind variability is thus a subtle interplay between variability originating in the corona, and turbulent evolution in-situ. Quantifying and understanding the fluctuating solar wind also provides an important input into models for the propagation of cosmic rays in the heliosphere, and for space weather for which the solar wind is the driver. The Sun's magnetic field is generated and maintained by a dynamo in the solar interior. Helioseismology offers a means by which we can probe beneath the visible surface of the Sun, constraining uncertain dynamo models and providing vital insights into the internal magnetic field that is ultimately responsible for the more readily observable manifestations in the solar atmosphere and beyond. The physics of warm dense matter is at an extreme boundary of our knowledge of plasma physics relevant to astrophysics. A quantitative understanding of these processes, closely coupled to observations, can be seen as either the means to understanding observed phenomena, such as cosmic rays, and the structure of gas giants, or as using the observed phenomena as a strong drive to understanding new fundamental plasma physics. These ideas, techniques and expertise that underpin this programme are thus of impact beyond plasma astrophysics.

对在太阳电晕和太阳风中作用的基本物理过程的定量理解不仅对太阳的物理及其与地球环境的联系至关重要，而且还增强了我们对天体物理等离子体过程的了解。冠状MHD波与太阳耀斑和喷发等许多动态具有直接相关性，并提供有关在其中运行的等离子体参数和物理过程的独特信息；冠状波能够将能量和机械动量从对流带转移到电晕和地球层中，并且与血浆不稳定性的发展有关。从太阳流出的血浆会产生太阳风。太阳风的质地和动力学与太阳电晕的质地和动力学密切相关，而这种高度可变的等离子体流可以导致局部加热，从而加速了太阳风。太阳风得到了加速，以至于原则上是湍流实验室，因此量化其波动对我们对湍流的理解有直接的影响。因此，太阳风变异性是源自电晕中的变异性与原位湍流进化之间的微妙相互作用。量化和理解波动的太阳风还为在地球球中传播宇宙射线的传播以及太阳风是驱动器的太空天气的模型提供了重要的输入。太阳的磁场是由太阳能内部发电机生成和维持的。 Helioseismology提供了一种方法，我们可以通过这种手段来探测太阳的可见表面，从而限制了不确定的发电机模型，并为内部磁场提供了重要的见解，最终导致了太阳大气中及其他地区更容易观察到的表现。温暖的物理物理学处于我们对与天体物理学相关的血浆物理学知识的极端边界。对这些过程的定量理解，与观察值紧密相结合，可以看作是理解观察到的现象的手段，例如宇宙射线和气体巨头的结构，或者用观察到的现象用作理解新的基本质量物理学的强大动力。因此，基于该计划的这些想法，技术和专业知识超出了血浆天体物理学的影响。

项目成果

Novel Data Analysis Techniques in Coronal Seismology

• DOI: 10.1007/s11214-021-00869-w
• 发表时间: 2021-12
• 期刊: Space Science Reviews
• 影响因子: 10.3
• 作者: S. Anfinogentov;P. Antolin;A. Inglis;D. Kolotkov;E. Kupriyanova;J. McLaughlin;G. Nisticò;D. Pascoe-D.-Pa

High-frequency Waves in Chromospheric Spicules

• DOI: 10.3847/1538-4357/ac5c53
• 发表时间: 2022-03
• 期刊: The Astrophysical Journal
• 作者: W. Bate;D. Jess;V. Nakariakov;S. Grant;S. Jafarzadeh;M. Stangalini;P. Keys;D. Christian

High Frequency Waves in Chromospheric Spicules

色球针状体中的高频波

• DOI: 10.48550/arxiv.2203.04997
• 发表时间: 2022
• 作者: Bate W

Bayesian evidence for two slow-wave damping models in hot coronal loops

热日冕环路中两种慢波阻尼模型的贝叶斯证据

• DOI: 10.1051/0004-6361/202346834
• 发表时间: 2023
• 期刊: Astronomy & Astrophysics
• 影响因子: 6.5
• 作者: Arregui I

Complex system perspectives of geospace electromagnetic environment research

地球空间电磁环境研究的复杂系统视角

• DOI: 10.5194/egusphere-egu2020-5070
• 发表时间: 2020
• 作者: Balasis G