Speaker
Description
The general understanding of oscillations in the Sun's atmosphere is that the photosphere is dominated by the global resonant modes of the entire stellar structure at 3mHz, while, moving upwards to the chromosphere, the dominant period shifts to 5mHz. However, the availability of stable and seeing-free coverage of the Sun for more than 15 years thanks to NASA’s Solar Dynamics Observatory (SDO) allowed us to carry out the largest statistical studies of the dynamics of magnetic structures in the photosphere. In our work, we tracked the horizontal perturbations of more than 1 million “small-scale” magnetic concentrations in the photosphere spanning a whole solar cycle and found a dominant frequency of 5mHz, unexpected at such heights. Furthermore, the analysis of the line-of-sight velocity of nearly 1 thousand sunspots highlighted the presence of statistically significant power in the 4-6mHz band. Understanding the origin of these frequencies, more commonly associated with chromospheric heights, is a challenging task that will require joint observation from multiple observatories, the help of numerical simulations and novel tools capable of working with the large datasets available. Our findings provide a timely avenue for future exploration of the magnetic connectivity between sub-photospheric, photospheric, and chromospheric layers of the Sun's dynamic atmosphere.
| Sessions | Wave generation, energy transport, dissipation and heating |
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