Fundamental astroplasma physics of the sun and heliosphere: Warwick Centre for Fusion Space and Astrophysics Rolling Grant Application

太阳和日光层的基本星形等离子体物理学：沃里克聚变空间和天体物理学中心滚动资助申请

• 批准号: ST/I000720/1
• 负责人: Sandra Chapman
• 金额: $ 158.44万
• 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: 2011
• 资助国家: 英国
• 起止时间: 2011 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FI000720%2F1
• 关键词: Fundamental; astroplasma; physics; sun; heliosphere

A 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. For instance, the chromosphere is a natural laboratory for studying the MHD of partially ionised plasmas. Coronal magnetohydrodynamic (MHD) waves are of direct relevance to much of the dynamics such as solar flares and eruptions; 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 solar wind is accelerated to such an extent that it is in principle an MHD turbulence laboratory so that quantifying its fluctuations has direct implications for our understanding of MHD turbulence. Recently, the solar wind has also been found to be a laboratory for a kinetic range of turbulence on scales below the ion gyrofrequency on which MHD no longer holds. Understanding this kinetic range physics is also highly relevant to our understanding of how the corona is heated. Quantifying and understanding the fluctuating solar wind provides an important input into models for the propagation of cosmic rays in the heliosphere, and for magnetospheric dynamics for which the solar wind is the driver. 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.

对太阳日冕和太阳风中的基本物理过程的定量了解不仅对太阳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一般知识。例如，色球层是研究部分电离等离子体MHD的天然实验室。日冕磁流体动力学（MHD）波与太阳耀斑和爆发等动力学有直接关系;日冕波能够将能量和机械动量从对流区转移到日冕和日光层，并与等离子体不稳定性的发展有关。太阳风被加速到这样的程度，它在原则上是一个MHD湍流实验室，因此量化其波动对我们理解MHD湍流有直接的影响。最近，太阳风也被发现是一个实验室的动力学范围内的湍流尺度低于离子回旋频率上的MHD不再持有。理解这种动力学范围的物理学也与我们理解日冕是如何被加热的高度相关。量化和了解波动的太阳风为日光层中宇宙射线传播模型和太阳风驱动的磁层动力学模型提供了重要的投入。在我们对等离子体物理学和天体物理学的相关知识中，热致密物质的物理学处于一个极端的边界。对这些过程的定量理解，与观测密切相关，可以被看作是理解观测现象的手段，如宇宙射线和气体巨星的结构，或者将观测到的现象作为理解新的基础等离子体物理学的强大动力。这些想法，技术和专业知识，支持这一计划，因此，影响超越等离子体天体物理学。

项目成果

THE DECAYING LONG-PERIOD OSCILLATION OF A STELLAR MEGAFLARE

恒星巨型耀斑的衰变长周期振荡

• DOI: 10.1088/0004-637x/773/2/156
• 发表时间: 2013
• 期刊: The Astrophysical Journal
• 作者: Anfinogentov S

Decay-less kink oscillations in coronal loops

• DOI: 10.1051/0004-6361/201322094
• 发表时间: 2013-12-01
• 期刊: ASTRONOMY & ASTROPHYSICS
• 影响因子: 6.5
• 作者: Anfinogentov, S.;Nistico, G.;Nakariakov, V. M.
• 通讯作者: Nakariakov, V. M.

Long-Period Oscillations of Sunspots by NoRH and SSRT Observations

NoRH 和 SSRT 观测的太阳黑子长周期振荡

• DOI: 10.1093/pasj/65.sp1.s13
• 发表时间: 2013
• 期刊: Publications of the Astronomical Society of Japan
• 影响因子: 2.3
• 作者: Bakunina I

A E , D S T , and Their SuperMAG Counterparts: The Effect of Improved Spatial Resolution in Geomagnetic Indices

A E 、 D S T 及其 SuperMAG 对应物：地磁指数空间分辨率提高的影响

• DOI: 10.1029/2020ja027828
• 发表时间: 2020
• 期刊: Space Physics
• 作者: Bergin A

Variation of geomagnetic index empirical distribution and burst statistics across successive solar cycles.

连续太阳周期中地磁指数经验分布和爆发统计的变化。

• DOI: 10.1002/essoar.10508033.1
• 发表时间: 2021
• 作者: Bergin A