Seismology of the solar corona with slow magnetoacoustic waves

慢磁声波日冕的地震学

• 批准号: 2737469
• 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: 2022
• 资助国家: 英国
• 起止时间: 2022 至 无数据
• 项目状态: 未结题
• 来源: https://gtr.ukri.org/projects?ref=studentship-2737469
• 关键词: Seismology; solar; corona; slow; magnetoacoustic

Modern spaceborne EUV imagers provide us with the confident detection of various kinds of magnetohydrodynamic (MHD) waves in plasma non-uniformities of the corona of the Sun. In particular, slow magnetoacoustic waves are manifested as propagating or standing field-aligned disturbances of the intensity of EUV emission or Doppler shifts of coronal emission lines, with typical observed or estimated speeds about the estimated sound speed. The aim of the project is to develop and apply novel methods of the seismological estimation of coronal heating function and/or transport coefficients and fine plasma structuring by the slow waves. In the project, the student will perform comprehensive analysis of propagating slow waves observed in plasma fan-like structures of coronal active regions and in plume structures in coronal holes. The attention will be paid to long-term variability of the wave parameters, such as instantaneous oscillation periods, apparent speeds and amplitudes, and their correlations with each other and parameters of waveguiding plasma non-uniformities. The required high-precision observational data will be obtained from the SDO/AIA and SolO/EUI archives. The data analysis will be supplemented by theoretical modelling in terms of MHD wave theory, accounting for the effect of wave-induced thermal misbalance.

现代星载极紫外成像仪为我们提供了可靠的探测日冕等离子体非均匀性中各种磁流体动力学（MHD）波的方法。特别地，慢磁声波表现为EUV发射强度或日冕发射线的多普勒频移的传播或驻波场对准扰动，具有关于估计声速的典型观察或估计速度。该项目的目的是开发和应用新的方法，对日冕加热函数和/或传输系数以及通过慢波进行精细等离子体结构化进行地震学估计。在该项目中，学生将对在日冕活动区的等离子体扇形结构和日冕洞中的羽流结构中观察到的传播慢波进行综合分析。注意将支付的波参数的长期变化，如瞬时振荡周期，视速度和振幅，以及它们之间的相互关系和波导等离子体非均匀性的参数。所需的高精度观测数据将从SDO/AIA和SolO/EUI档案中获得。数据分析将由MHD波理论的理论建模来补充，解释波引起的热不平衡的影响。