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UK APAP Network

英国APAP网络

基本信息

批准号：
ST/V000683/1
负责人：
Nigel Badnell
金额：
$ 49.47万
依托单位：
University of Strathclyde
依托单位国家：
英国
项目类别：
Research Grant
财政年份：
2021
资助国家：
英国
起止时间：
2021 至无数据
项目状态：
未结题

来源：
https://gtr.ukri.org/projects?ref=ST%2FV000683%2F1
关键词：
UK APAP Network

项目摘要

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, XRISM, \& ATHENA 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 calculatedand incorporated into atomic databases of plasma models.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.In X-ray astrophysics, we still have gaps in our understanding of outflows in active galactic nuclei,especially the density of the outflows. This limits our estimation of the kinetic power, thus, the impactof the outflows to the host galaxy.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.We will also development of the photoionized plasma model in SPEX toenable density diagnostics of N-like to F-like ions with metastable absorption lines. We will analyzeX-ray low-energy grating spectra to quantify the density and power of ionized outflows in activegalactic nuclei.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.

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，XRISM，\和ATHENA将提供没有放松。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，面对观测。此外，恒星内部的地震学，包括我们的太阳，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并将其纳入等离子体模型的原子数据库。这可能令人惊讶，但是离子产生的大部分光谱仍然没有被探索。观测和理论之间仍然存在很大的差异。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，（天体物理学和实验室）等离子体。此外，还有一个长期存在的问题，关于我们的太阳元素丰度。这被认为是由于我们不完全了解如何从它的内部深处发出微弱的光。在X射线天体物理学中，我们对活动星系核外流的理解仍有差距，特别是外流的密度。这限制了我们对动能的估计，从而限制了外流对宿主星系的影响。我们提出的计算将使卫星和恒星地震学的光谱数据的解释成为可能，这将进一步加深我们对日冕，恒星大气，超新星遗迹，我们还将在dac中发展光电离等离子体模型，以实现类N到F的密度诊断。比如具有亚稳态吸收线的离子。我们将通过分析X射线低能光栅谱来量化活动星系核中电离外流的密度和功率，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。