S. Jafarzadeh, L. A. C. A. Schiavo, V. Fedun, S. K. Solanki, M. Stangalini, D. Calchetti, G. Verth, D. B. Jess, S. D. T. Grant, I. Ballai, R. Gafeira, P. H. Keys, B. Fleck, R. J. Morton, P. K. Browning, S. S. A. Silva, T. Appourchaux, A. Gandorfer, L. Gizon, J. Hirzberger, F. Kahil, D. Orozco Suárez, J. Schou, H. Strecker, J. C. del Toro Iniesta, G. Valori, R. Volkmer, J. Woch
Abstract
Solar pores are intense concentrations of magnetic flux that emerge through the solar photosphere. When compared to sunspots, they are much smaller in diameter and can therefore be affected and buffeted by neighbouring granular activity to generate significant magnetohydrodynamic (MHD) wave energy flux within their confines. However, observations of solar pores from ground-based telescope facilities may struggle to capture subtle motions that are synonymous with higher-order MHD wave signatures because of the seeing effects that are produced in the Earth’s atmosphere. Hence, we exploited timely seeing-free and high-quality observations of four small magnetic pores from the High Resolution Telescope (HRT) of the Polarimetric and Helioseismic Imager (PHI) on board the Solar Orbiter spacecraft during its first close perihelion passage in March 2022 (at a distance of 0.5 au from the Sun). Through acquisition of data under stable observing conditions, we were able to measure the area fluctuations and horizontal displacements of the solar pores. Cross correlations between perturbations in intensity, area, line-of-sight velocity, and magnetic fields, coupled with the first-time application of novel proper orthogonal decomposition techniques on the boundary oscillations, provided a comprehensive diagnosis of the embedded MHD waves as sausage and kink modes. Additionally, the previously elusive m = 2 fluting mode is identified in the most magnetically isolated of the four pores. An important consideration lies in how the identified wave modes contribute to the transfer of energy into the upper solar atmosphere. Approximately 56%, 72%, 52%, and 34% of the total wave energy of the four pores we examined is associated with the identified sausage modes and about 23%, 17%, 39%, and 49% with their kink modes, while the first pore also receives a contribution of about 11% linked to the fluting mode. This study reports the first-time identification of concurrent sausage, kink, and fluting MHD wave modes in solar magnetic pores.
Keywords
magnetohydrodynamics (MHD) / Sun: magnetic fields / Sun: oscillations / Sun: photosphere
Notes
Movies associated to Fig. 8 are available at https://www.aanda.org.
Astronomy & Astrophysics
Volume 688, Article Number A2, Number of pages 12
2024 August
