The Role of MHD Waves in Coronal Heating

我们将研究发生在日冕环足点的色球蒸发的影响。这将通过使用Lare2d代码求解一组MHD方程的2.5 d模拟来实现。日冕环被建模为“直环”，最初处于磁流体静力平衡状态。这种“直环”模型被观测到的日冕环的小纵横比证明是正确的。与周围的日冕等离子体相比，日冕环被建模为密度增强的区域。与日冕区相比，色球层被建模为密度增强的区域。然后，我们将在这个基本模型中研究alfvsamn波的传播和耗散。我们将考虑不同周期的驱动范围以及不同振幅和波激励的位置。我遵循圣安德鲁斯大学对新PGR学生的入职计划。除此之外，我还将学习由数学与统计学院组织的定向阅读和计算技能课程/项目。

We will examine the effect of chromospheric evaporation occurring at the footpoints of a coronal loop. This will be achieved with a 2.5-D simulation using the Lare2d code to solve the set of MHD equations. The coronal loop is modelled as a 'straight loop', initially in a magnetohydrostatic equilibrium. This 'straight loop' model is justified by the small aspect ratio of observed coronal loops. The coronal loop is modelled as an area of enhanced density compared to the surrounding coronal plasma. The chromosphere is modelled as an area of enhanced density when compared with the coronal region. We will then examine the propagation and dissipation of Alfvén waves in this basic model. We will consider a range of different periods for the driver as well as different amplitudes and location of the wave excitation. I am following the University of St Andrews' induction plan for new PGR students. Alongside this I will be following a course of directed reading and computational skills/projects organised by the School of Mathematics and Statistics.