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（太阳）和Chandra、XMM-牛顿、HST等卫星任务中获得了大量的XUV光谱数据，保险丝（非太阳）。每个物体中的物质状态-温度和密度的分布、化学成分、流速-可以通过光谱数据的诊断分析来确定，在光谱数据中，模型结合了物体的全部物理特性，面对观察。这些信息对于我们理解宇宙的起源和演化至关重要。电子和光子与原子，离子和分子的碰撞在表征天体物理等离子体中起着重要作用，因此有必要计算精确的原子数据。这可能令人惊讶，但是离子产生的光谱中有很大一部分还没有被探索，观测和理论之间的巨大差异也仍然存在。近年来，为了解决电子-离子碰撞谱线强度计算值和计算值之间长期存在的巨大差异，我们已经证明了对单个离子进行精确计算的必要性。（天体物理和实验室）等离子体。我们提出了一系列的计算，这将使我们能够解释这些卫星的光谱数据，这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通过这一提议，我们的目标是加强实验，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、可靠和环境友好能源的追求。

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, in particular in the spectrallines that are emitted by the ions that are present in the plasmas.In recent years, an overwhelming amount of XUV spectroscopic data have been obtained from the satellite missionssuch as SOHO, Hinode, STEREO, SDO (solar) and Chandra, XMM-Newton, HST, FUSE (non-solar).The state of matter in each object --- the distribution of temperature and density, chemical composition,flow velocities --- can be determined through diagnostic analysis of spectral data in which models,incorporating the full physics of the object, confront the observations. This information is 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 in characterizing 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 of electron-ioncollisions for individual ions, in order to solve the large, long-standing discrepancies between observedand calculated line intensities in collisional (astrophysical and laboratory) plasmas.We propose a series of calculations which will enable us to interpret spectral data from these satelliteswhich will further our understanding of the solar corona, stellar atmospheres, supernova remnants, nebulae and stars. With this proposal, we aim to strengthen the collaboration between experimental, observational and theoretical research. Our work will also impact upon the magnetic fusion program and its quest for asafe, reliable and environmentally friendly energy source.