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Data-constrained Modeling of the Flaring Solar Chromosphere

耀斑太阳色球层的数据约束建模

基本信息

批准号：
2445972
负责人：
金额：
--
依托单位：
Queen's University Belfast
依托单位国家：
英国
项目类别：
Studentship
财政年份：
2020
资助国家：
英国
起止时间：
2020 至无数据
项目状态：
已结题

来源：
https://gtr.ukri.org/projects?ref=studentship-2445972
关键词：
Data constrained Modeling Flaring Solar

项目摘要

The Sun, our nearest star, has a profound influence on all life on Earth. As we become more and more reliant upon technology, understanding how the Sun's radiative output varies, and the impact of that variability on planetary atmospheres, is becoming ever more important through the emerging field of space weather research. The Sun's output can vary on a range of timescales, from seconds to minutes (during solar flares), to weeks and months (due to sunspot rotation), and years and decades (over solar cycles). Solar flares are the most energetic explosions in the solar system resulting from rapid restructuring of the Sun's coronal magnetic field. This accelerates particles to extremely high energies which ultimately collide with the dense, underlying chromosphere, causing it to heat and expand. The resulting increase in ultraviolet and X-ray radiation can significantly impact the upper layers of Earth's atmosphere, as well as those of other planets. On Earth this can have implications for GPS accuracy, the propagation of radio signals, and atmospheric drag on orbiting spacecraft. This radiation also allows us to diagnose the plasma conditions within the flaring chromosphere itself and put constraints on various flare heating models, as the underlying physical mechanisms are not yet fully understood. The study of solar flares is also important to help us understand flares on other stars, and how they may impact the search for potentially habitable exoplanets.As Solar Cycle 24 draws to a close, a considerable amount of solar flare data has been amassed from a wealth of space-based solar observatories over the past decade. Numerical simulations of solar flare heating have also become more sophisticated thanks to advances in computation. These two factors make this an opportune time to make significant strives in our understanding of what drives increases in ultraviolet radiation during solar flares, how this contributes to the solar irradiance, and what impact this has on planetary atmospheres. As we look ahead to Solar Cycle 25 this research will also be crucial for the interpretation of observations from newly-launched and upcoming space missions that will study the Sun in greater detail than ever before.

太阳是离我们最近的星星，对地球上的所有生命都有着深远的影响。随着我们越来越依赖技术，通过新兴的空间气象研究领域，了解太阳辐射输出的变化以及这种变化对行星大气的影响变得越来越重要。太阳的输出可以在一系列时间尺度上变化，从几秒到几分钟（在太阳耀斑期间），到几周和几个月（由于太阳黑子旋转），以及几年和几十年（在太阳周期中）。太阳耀斑是太阳系中能量最大的爆炸，是由于太阳日冕磁场的快速重组而产生的。这将粒子加速到极高的能量，最终与致密的底层色球层相撞，导致它加热和膨胀。由此产生的紫外线和X射线辐射的增加可以显著影响地球大气层的上层，以及其他行星的大气层。在地球上，这可能会影响GPS的准确性、无线电信号的传播以及轨道航天器上的大气阻力。这种辐射还使我们能够诊断耀斑色球层本身内的等离子体条件，并对各种耀斑加热模型进行限制，因为其基本的物理机制尚未完全了解。对太阳耀斑的研究对于帮助我们了解其他恒星上的耀斑以及它们如何影响对潜在可居住系外行星的搜索也很重要。随着太阳活动周期24接近尾声，在过去十年中，大量的太阳耀斑数据已经从大量的空间太阳观测站积累起来。由于计算技术的进步，太阳耀斑加热的数值模拟也变得更加复杂。这两个因素使这是一个适当的时机，使我们在理解太阳耀斑期间紫外线辐射增加的原因，这如何有助于太阳辐照度以及这对行星大气的影响方面做出重大努力。当我们展望第25个太阳活动周期时，这项研究对于解释新发射和即将发射的太空任务的观测结果也至关重要，这些任务将比以往任何时候都更详细地研究太阳。