Effects of flares on solar high-degree helioseismic acoustic mode amplitudes

Several attempts have been made to observe whether solar flares excite acoustic modes since Wolff (1972) suggested this possibility. Moreover, the rapid progress of asteroseismology and the study of stellar flares makes the study of these phenomena in the Sun important to inform our study of the influence of the more energetic stellar flares on asteroseismic acoustic modes. We look for the impact of flares on the amplitude of solar acoustic modes and other effects that are also affecting the mode amplitude. Solar acoustic mode amplitudes are known to be sensitive to magnetic fields. As flares usually occur in the presence of strong magnetic fields and most likely are the by-product of magnetic reconnection, we show how the magnetic field in and around the flaring region affects the mode amplitude. The mode amplitudes were obtained using ring-diagram analysis, which was first applied to a single event, the largest flare in the space age (the `Halloween Flare', SOL2003-10-28T11:00), using MDI data. Then, using HMI data, the analysis was applied to the regions corresponding to the flares observed during the high activity phase of cycle 24 and that fall into two groups. These two groups consist of small (10-60 erg cm$^{-2}$ s$^{-1}$) and large ($>$1200 erg cm$^{-2}$ s$^{-1}$) peak-flux flares, based on the Heliophysics Event Knowledgebase (HEK). After applying several corrections in order to take into account several sources of bias, we did not find any amplification in the inferred mode amplitude due to flaring activity, within a 10% uncertainty.