Magnetohydrodynamic wave interaction with flows in the Sun's chromosphere

磁流体动力波与太阳色球层中流动的相互作用

• 批准号: 2881442
• 金额: --
• 依托单位: University of Warwick
• 依托单位国家: 英国
• 项目类别: Studentship
• 财政年份: 2023
• 资助国家: 英国
• 起止时间: 2023 至 无数据
• 项目状态: 未结题
• 来源: https://gtr.ukri.org/projects?ref=studentship-2881442
• 关键词: Magnetohydrodynamic; wave; interaction; flows; Sun

The Sun is our nearest star with a direct impact on life and technology on Earth. Space-born and ground-based instruments have confirmed the ubiquitous presence of magnetohydrodynamic (MHD) waves throughout its atmosphere. They provide insight into the major unanswered questions of solar physics. MHD waves are capable of transferring energy and mechanical momentum from the convection zone into the corona and heliosphere. They are often associated with space weather activity such as solar flares and coronal mass ejections. Owing to the great success of MHD wave theory, we possess a diagnostic tool to extract detailed, local knowledge of physical conditions in the solar atmosphere. The UK, and the University of Warwick in particular, are internationally recognised leaders in this field. This project lends itself to a holistic approach that combines observational analysis, theoretical and numerical modelling.With the recent inauguration of the new ground-based Daniel K. Inouye Solar Telescope (DKIST), with its unprecedented resolution, there is a renewed focus on chromospheric dynamics. This project will study the occurrence of MHD waves in chromospheric structures such as flare ribbons and swirls. Flare ribbons are chromospheric regions of heating due to magnetic reconnection events higher-up. They are accompanied by a variety of wave activity such as fast waves that ripple across ribbons as well as acoustic shocks propagating up. In particular, the project will focus on the role of inflows on the strength of wave dynamics and transport of energy and momentum into the upper chromosphere.

太阳是离我们最近的星星，对地球上的生命和技术有直接影响。空间和地面仪器已经证实了磁流体动力学（MHD）波在整个大气中无处不在。它们提供了对太阳物理学主要未解问题的深入了解。MHD波能够将能量和机械动量从对流区转移到日冕和日光层。它们往往与太阳耀斑和日冕物质抛射等空间气象活动有关。由于MHD波理论的巨大成功，我们拥有一个诊断工具，以提取详细的，本地的知识，在太阳大气中的物理条件。英国，特别是沃里克大学，是这一领域国际公认的领导者。该项目采用了一种综合方法，将观测分析、理论和数值模拟结合起来。Inouye太阳望远镜（DKIST）以其前所未有的分辨率，重新关注色球动力学。本计画将研究磁流体动力学波在色球结构中的发生，例如耀斑带和漩涡。耀斑带是色球层因高层磁场重联事件而产生的加热区域。它们伴随着各种各样的波活动，例如在带状物上涟漪的快波以及向上传播的声震。特别是，该项目将侧重于流入对波动强度的作用以及能量和动量向上层色球层的输送。