Modelling Elementary Coronal Heating Events

光球层的对流驱动可以产生进入太阳大气的坡印亭通量，足以为日冕加热提供动力。与当地阿尔芬速度相比速度较慢的司机会在大气磁场中产生压力，这些压力可以在重新连接事件期间释放。另一方面，速度更快的司机会导致波动。使用数值程序Lare3D，我们计划开发考虑连续驱动对(组)磁通量管的影响的日冕模型。我们将包括热传导，以确定热是如何重新分布的，并考虑其对等离子体和磁场的影响。此外，我们还研究了辐射冷却在加热时间尺度上的大小，以帮助建立所提出的加热机制的有效性。将使用正向建模来为当前和未来的仪器得出可观测数据。培训-+大学范围内的新博士生入职培训+新教师的大学入门课程+圣安德鲁斯太阳能集团入职课程，包括前3个月的指导阅读和3个迷你项目+太阳能集团每周研讨会课程+MPI课程

The convective driving of the photosphere can generate a Poynting Flux into the solar atmosphere that is sufficient to power coronal heating. A driver that is slow in comparison to the local Alfvén speed will build stresses in the atmospheric magnetic field, which can be released during reconnection events. A faster driver on the other hand, will lead to wave motions. Using the numerical code Lare3D, we plan to develop coronal models that considers the effects of continuous driving on (sets of) magnetic flux-tubes. We will include thermal conduction to determine how heat is re-distributed and consider its effects on both the plasma and the magnetic field. Further we investigate the magnitude of radiative cooling on the heating timescale in order to help establish the efficacy of the proposed heating mechanism. Forward modelling will be used to derive observables for current and future instrumentation.Training -+ University wide induction for new PhD students+ University induction sessions for new tutors+ St Andrews Solar Group induction programme consisting of guided reading and 3 mini projects during the first 3 months+ Solar Group weekly seminar programme+ Course on MPI