Fundamental plasma physics of the sun and heliosphere: CFSA Warwick

定量了解太阳日冕和太阳风的基本物理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，而且还增强了我们对天体物理等离子体过程的总体认识。例如，色球层是研究部分电离等离子体磁流体动力学（MHD）的天然实验室。日冕MHD波与许多动力学直接相关，如太阳耀斑和喷发，并携带有关等离子体参数和在其中运行的物理过程的独特信息；日冕波能够将能量和机械动量从对流区传递到日冕和日球层，并与等离子体不稳定性的发展有关。从太阳流出的等离子体产生太阳风。太阳风的结构和动力学与日冕的结构和动力学密切相关，这种高度可变的等离子体流可以导致局部加热，从而加速太阳风。太阳风被加速到这样的程度，原则上它是一个湍流实验室，因此量化它的波动对我们对湍流的理解有直接的影响。量化和理解太阳风的波动也为宇宙射线在日球层中的传播模型和磁层动力学（包括以太阳风为驱动因素的空间天气）提供了重要的输入。太阳的磁场是由太阳内部的发电机产生和维持的。日震学提供了一种手段，使我们能够探测到可见的太阳表面之下，限制不确定的发电机模型，并提供对内部磁场的重要见解，而内部磁场最终导致了太阳大气层内外更容易观察到的现象。热致密物质的物理学是我们与天体物理学相关的等离子体物理学知识的一个极端边界。对这些过程的定量理解，与观测密切相关，可以被视为理解观测到的现象（如宇宙射线和气体巨星的结构）的手段，或者将观测到的现象作为理解新的基本等离子体物理学的强大动力。因此，支撑这个项目的这些想法、技术和专业知识的影响超出了等离子体天体物理学。

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 magnetohydrodynamic (MHD) of partially ionised plasmas. 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.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 magnetospheric dynamics including 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.