UK APAP Network

等离子体遍布我们的宇宙，存在于恒星大气、星系中的星际气体云、行星状星云、超新星遗迹、黑洞吸积盘等等。所有这些物体的光谱学显示了丰富的信息，特别是在等离子体中存在的离子发射的光谱线中。近年来，大量的XUV光谱数据已经从诸如SOHO、Hinode、STEREO、SDO、IRIS（太阳）和钱德拉、xmm -牛顿、HST、FUSE（非太阳）等卫星任务中获得，而即将到来的和未来的任务，如太阳轨道器，将提供不间断的数据。每个物体中的物质状态——温度和密度的分布、化学成分——可以通过对光谱数据的诊断分析来确定，在这种分析中，模型结合了物体的全部物理特性，与观测结果相对应。此外，恒星内部的地震学，包括我们的太阳，是对其结构的独特探索。光谱学和地震学信息是我们理解宇宙起源和演化的基础。电子和光子与原子、离子和分子的碰撞在天体物理等离子体的特征中起着基本作用，因此有必要计算准确的原子数据。这可能令人惊讶，但离子产生的光谱的很大一部分仍未被探索。观测和理论之间的巨大差异仍然存在。近年来，我们已经证明需要对单个离子的电子-离子碰撞进行精确计算，以解决碰撞等离子体（天体物理和实验室）中观测到的和计算得到的线强度之间长期存在的巨大差异。此外，还有一个长期存在的问题是关于我们太阳的元素丰度。这被认为是由于我们对低光如何从其内部深处出现的理解不完全。我们提出的计算将能够解释来自卫星和恒星地震学的光谱数据，这将进一步加深我们对太阳日冕、恒星大气、超新星遗迹、星云和恒星的理解。通过这一建议，我们旨在加强实验、观测和理论研究之间的合作。我们的工作也将对磁融合计划及其对安全、可靠和环保能源的追求产生影响。

Plasmas permeate our Universe, being present in stellar atmospheres, interstellar gas clouds in galaxies, planetary nebulae, supernova remnants, black hole accretion disks, and so on.Spectroscopy of all these objects has shown a richness of information, inparticular in the spectral lines that are emitted by the ions that are present in the plasmas.In recent years, an overwhelming amount of XUV spectroscopic data have beenobtained from the satellite missions such as SOHO, Hinode, STEREO, SDO, IRIS (solar) and Chandra, XMM-Newton, HST, FUSE(non-solar), while upcoming and future missions such as Solar Orbiter will provide no let-up.The state of matter in each object --- the distribution of temperature and density, chemical composition --- can be determined through diagnostic analysis of spectral data in which models, incorporating the full physics of the object, confront the observations.In addition, seismology of stellar interiors, including our sun, are a unique probe of their structure.Spectroscopy and seismology information are fundamental for our understanding of the origin and evolution of the Universe.Collisions of electrons and photons with atoms, ions and molecules play a fundamental role incharacterizing astrophysical plasmas, and it is therefore necessary that accurate atomic data are calculated.It might be surprising, but a large fraction of the spectra produced by ions is still unexplored.Large discrepancies between observations and theory are also still present.In recent years, we have shown the need to perform accurate calculations ofelectron-ion collisions for individual ions, in order to solve the large, long-standingdiscrepancies between observed and calculated line intensities in collisional (astrophysical and laboratory) plasmas.Furthermore, there is also a long standing problem concerning the elemental abundance of our sun.It is thought to be due to our incomplete understanding of how low light emerges from deep in its interior.We propose calculations which will enable the interpretation of spectraldata from satellites and stellar seismology which will further our understanding of the solar corona, stellar atmospheres,supernova remnants, nebulae and stars.With this proposal, we aim to strengthen the collaboration betweenexperimental, observational and theoretical research. Our work will also impact upon the magnetic fusionprogram and its quest for a safe, reliable and environmentally friendly energy source.