Videos of p-Mode Oscillations in Highly Gravitationally Stratified Magnetic Solar Atmospheres

The solar atmosphere exhibits a diverse range of wave phenomena, one of the earliest to be discovered was the five minute oscillation, the p-mode. The analysis of wave propagation in the solar atmosphere may be used as a diagnostic tool to measure the physical characteristics of the solar atmosphere.The videos in this collection are the result of an investigation of the dynamics and propagation of waves which are generated by the solar global eigenmodes. We present the results of a series of MHD simulations of a realistic model of the solar atmosphere with a vertically uniform cylindrically symmetric magnetic field. With the objective of recreating atmospheric motions generated by global resonant oscillation the simulations use a driver which is spatially structured and extended in a sinusoidal profile across the computational model. The drivers perturb the region at 0.5Mm above the bottom boundary of the model and coincident with the temperature minimum. A combination of the VALIIIC and McWhirter solar atmospheres and coronal density profiles were used as the background equilibrium model in the simulations. We present the results of a study of synthetic photospheric oscillations for a quiet solar atmosphere with a vertically uniform cylindrically symmetric magnetic. To carry out the simulations, we employed the MHD code, SMAUG (Sheffield MHD Accelerated Using GPUs).Each video shows the value of the vertical component of the plasma velocity (z-component) along different slices through the simulation box. The scale shows the velocity value in m/s. The simulation box is 4Mmx4Mm along the base and the height of the box is 5.7Mm. The driver for the simulations is located at a height of 0.5Mm.The videos are for a (2,2) mode driver with a period of 300s each video is labelled with field strength at the centre of the box i.e. 0G, 50G, 75G and 100G. The magnetic field lines are shown in blue running vertically, contours illustrate the cylindrical magnetic field.

太阳大气层展现出了丰富多彩的波动现象，其中最早被发现之一即为五分钟振荡，即p模。对太阳大气层中波动传播的分析可作为一种诊断工具，用以测量太阳大气的物理特性。本数据集中的视频是研究由太阳全局本征模态产生的波动动力学和传播的结果。我们展示了基于具有垂直均匀、圆柱对称磁场真实模型太阳大气层的一系列磁流体动力学（MHD）模拟结果。为了重现由全局共振振荡产生的大气运动，模拟采用了空间结构化且沿计算模型呈正弦分布的驱动器。驱动器扰动模型底部边界以上0.5兆米的区域，与温度最小值相吻合。在模拟中，我们使用了VALIIIC和McWhirter太阳大气层以及日冕密度分布作为背景平衡模型。我们展示了针对具有垂直均匀、圆柱对称磁场的宁静太阳大气层合成的光球振荡研究的结果。为了执行这些模拟，我们采用了磁流体动力学代码SMAUG（利用GPU加速的谢菲尔德MHD）。每个视频展示了通过模拟盒子不同切片的等离子体速度垂直分量（z分量）的值。刻度显示了速度值（单位：米每秒）。模拟盒子在底部沿4兆米×4兆米的长度上，盒子的高度为5.7兆米。模拟驱动器位于0.5兆米的高度。视频针对的是周期为300秒的(2,2)模态驱动器，每个视频都标有盒子中心的磁场强度，即0G、50G、75G和100G。磁场线用蓝色垂直表示，等高线描绘了圆柱形磁场。