Fundamental Plasma Physics of the Solar System: Warwick CFSA Rolling Grant Application

太阳系基础等离子体物理学：Warwick CFSA 滚动资助申请

• 批准号: ST/F00205X/1
• 负责人: Sandra Chapman
• 金额: $ 156.62万
• 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: 2008
• 资助国家: 英国
• 起止时间: 2008 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FF00205X%2F1
• 关键词: Fundamental; Plasma; Physics; Solar; System

We request support for a programme of research within three themes: (i) coronal dynamics (ii) solar wind turbulence and (iii) plasma phenomena for astrophysics. A quantitative understanding of the fundamental physical processes acting in the corona, in particular processes responsible for the energy release in flares, heating the corona and accelerating the 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 plasmas processes in general. For instance, the corona is a laboratory for studying magnetic reconnection in three dimensions. Coronal 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, with magnetic Reynolds number estimated as ~ 10^5 is in principle an MHD turbulence laboratory so that quantifying its fluctuations has direct implications for our understanding of MHD turbulence; it is also highly relevant to our understanding of coronal heating (of which we see a remnant signature in the solar wind), of the propagation of cosmic rays in the heliosphere, and magnetospheric dynamics for which the solar wind is the driver. Particle acceleration by collisionless shocks, and the physics of warm dense matter, are at two extreme boundaries of our knowledge of plasma physics relevant to astrophysics. A quantitative understanding of these processes, closely coupled to observations, can again be seen as either the means to understanding observed phenomena, namely cosmic rays, and the structure of gas giants, or as using the observed phenomena as a strong drive to understanding new fundamental plasma physics.

我们要求支持三个主题中的研究计划：（i）冠状动脉动力学（II）天体物理学的太阳风湍流和（iii）血浆现象。对作用在电晕作用的基本物理过程的定量理解，特别是导致耀斑能量释放，加热电晕并加速太阳风的过程，不仅对太阳的物理学及其与地球环境的联系至关重要，而且还可以增强我们对天体血浆过程的知识。例如，电晕是研究三个维度的磁重新连接的实验室。冠状MHD波与太阳耀斑和爆发等许多动力学有直接相关。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。据估计为〜10^5的磁性雷诺数的太阳风原则是MHD湍流实验室，因此量化其波动的直接影响对我们对MHD湍流的理解具有直接影响。这也与我们对冠状加热的理解高度相关（我们在太阳风中看到了残留的签名），地球层中宇宙射线的传播以及太阳风是驱动器的磁层动力学。通过无碰撞冲击和温暖的物理物理学加速粒子在我们对与天体物理学相关的血浆物理学知识的两个极端边界处。对这些过程的定量理解，与观察结果紧密结合，可以再次将其视为理解观察到的现象，即宇宙射线和气体巨头的结构，或者将观察到的现象用作理解新的基本血浆物理学的强大动力。

项目成果

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

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 microwave emission of solar active regions: observations with NoRH and SSRT

太阳活动区微波发射的长周期振荡：NoRH 和 SSRT 观测

• DOI: 10.1017/s1743921309029214
• 发表时间: 2008
• 期刊: Proceedings of the International Astronomical Union
• 作者: Bakunina I

THERMAL FRONTS IN FLARING MAGNETIC LOOPS

喇叭形磁环中的热锋

• DOI: 10.1088/0004-637x/690/1/238
• 发表时间: 2009
• 期刊: The Astrophysical Journal
• 作者: Arber T