The Role of MHD Waves in Coronal Heating

我们将研究色球层蒸发在冕环足点处发生的效应。这将通过使用Lare 2d代码求解MHD方程组的2.5-D模拟来实现。日冕环被模拟为一个“直环”，最初在磁流体静力平衡。这种“直环”模型是合理的观测冠状环的小纵横比。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。色球层被模拟为一个区域的密度增强相比，日冕区域。然后，我们将研究阿尔文波在这个基本模型中的传播和耗散。我们将考虑驱动器的不同周期范围以及波激励的不同振幅和位置。我正在遵循圣安德鲁斯大学为新PGR学生制定的入职计划。除此之外，我将遵循由数学与统计学院组织的定向阅读和计算技能/项目课程。

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.