A Topic in Coronal Heating

日冕加热问题，即理解太阳日冕是如何被加热到比太阳表面高出许多量级的温度的，仍然是天体物理学中的一个突出问题。这个问题已经存在了80多年，最近的进展是由于观测的改进和更严格和更复杂的计算机模型的发展。阿尔芬波的相位混合长期以来一直被认为是一种可能的日冕加热机制。Van Damme最近的一篇论文利用磁流体力学(MHD)模拟研究了Alfvén波的位相混合引起的加热如何定量地影响蒸发，以及这种蒸发如何影响横向密度分布。研究得出的结论是，由于所选择的初始条件，对密度梯度的影响不大。这个项目将在这项工作的基础上展开，使用Lare2D程序来研究蒸发如何影响密度分布。

The problem of Coronal Heating, understanding how the solar corona is heated to a temperature many magnitudes greater than that of the solar surface, remains an outstanding problem in astrophysics. This problem has existed for over 80 years, with recent advancements driven by improved observations and the development of more rigorous and sophisticated computer models.The phase mixing of Alfvén waves has long been suggested as a possible coronal heating mechanism. A recent paper by Van Damme used magnetohydrodynamic (MHD) simulations to investigate how heating caused by the phase-mixing of Alfvén waves quantitatively affects evaporation, and how this evaporation may influence the transverse density profile. The study concluded that due to the initial conditions selected , there was only an insignificant impact upon the density gradient. This project will begin by expanding upon this work, using the Lare2D code to study how evaporation may impact the density profile.