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.