Mathematical modelling of MHD instabilities in solar jet structures

致力于太阳等离子体中开尔文-亥姆霍兹和瑞利-泰勒的观测、数值和分析研究。通过分析Hinode卫星上的太阳光学望远镜数据（Ca II谱线）和瑞典太阳望远镜的地面数据，从观测上确定RT不稳定性的出现状态、其形态和寿命。- 数值模拟射流状结构，特别关注与磁场强度和方向相关的过程，以分析由于有效加速而导致的射流顶部RT不稳定性的出现和发展。此外，调查过程中发生的开尔文-亥姆霍兹（KH）不稳定性射流的演变。- 在存在磁场的情况下，解析地获得RT和KH不稳定性的条件（例如，通过使用自相似方法建模），并将其应用于前面讨论的观测和数值数据。分析波激励（包括Alfven在内的MHD波）及其直接由于喷流传播而产生的能量收支。

working on observational, numerical and analytical studies of the Kelvin-Helmholtz and Rayleigh-Taylor in solar plasma. In particular:- observationally identify regimes of appearance of the RT instability, its morphology and lifetime by analysing Solar Optical Telescope data (Ca II spectral lines) on board the Hinode satellite and ground-based data from the Swedish Solar Telescope (SST). - numerically model jet like structures, with particular interest in processes related to the magnetic field strength and direction to analyse the appearance and development of the RT instability at the top part of the jet due-to effective acceleration. Additionally, investigate processes related to the Kelvin-Helmholtz (KH) instability taking place during the evolution of the jet. - analytically obtain conditions for RT and KH instabilities in the presence of a magnetic field (for example modeled by using self-similar approach) and apply them to the observational and numerical data discussed in the previous points.- analysis of wave excitation (MHD waves including Alfven) and their energy budget directly due to jet propagation.