UK APAP Network

等离子体遍布我们的宇宙，存在于恒星大气层，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。所有这些物体的光谱学都显示出丰富的信息，特别是在等离子体中存在的离子发射的光谱线中。近年来，从SOHO、Hinode、STEREO、SDO、IRIS（太阳）和Chandra、XMM-牛顿、HST、FUSE等卫星任务中获得了大量的XUV光谱数据（非太阳），而即将到来的和未来的任务，如太阳轨道器将提供没有松懈。在每个对象的物质状态-温度和密度的分布，化学成分--可以通过诊断分析光谱数据，其中模型，结合天体的全部物理学，面对观测。此外，恒星内部的地震学，包括我们的太阳，是它们结构的独特探测器。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描述天体物理等离子体中起着基础作用，因此，计算精确的原子数据是必要的。这可能是令人惊讶的，但离子产生的光谱的很大一部分仍然没有探索。观测和理论之间的巨大差异也仍然存在。近年来，我们已经表明需要对单个离子进行精确的电子-离子碰撞计算，为了解决在碰撞中观测到的和计算出的谱线强度之间长期存在的巨大差异，（天体物理和实验室）等离子体。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太阳内部深处发出的微弱光线的不完全理解。我们提出了能够解释这一问题的计算方法。通过卫星和恒星地震学的光谱数据，将进一步加深我们对日冕、恒星大气、超新星遗迹、星云和恒星的了解。通过这一提议，我们旨在加强实验、观测和理论研究之间的合作。我们的工作也将影响磁聚变计划及其对安全，可靠和环保能源的追求。

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.