Speaker
Description
Solar flares are characterized by rapid enhancements in electromagnetic emission across multiple wavelengths. This study investigates the extreme ultraviolet (EUV) emission associated with the X8.2-class solar flare that occurred near the solar limb on 10 September 2017 in active region NOAA 12673. The region exhibited a 𝛽𝛾 magnetic configuration with interacting opposite-polarity flux systems and multiple polarity inversion lines. EUV observations obtained between 13:00 and 19:00 UT indicate that the plasma was initially confined within a complex magnetic topology connecting distinct photospheric regions. Prior to flare onset, the coronal structure evolved quasi-statically, followed by a dynamic magnetic reconfiguration that produced a post-flare loop arcade. A precursor plasma jet was detected before the eruption, and observations in the 94 Å and 131 Å channels revealed a filamentary structure consistent with a possible current sheet. Light-curve analysis shows an initial emission enhancement at approximately 15:45 UT associated with the jet, followed by a rapid increase culminating in a primary peak near 16:07 UT. Wavelet analysis identified short-period oscillations superimposed on the EUV emission from jet initiation through the onset of the decay phase. The mean vertical emission profile indicates upward propagation of the dominant emission source to heights of approximately 42 Mm, accompanied by a progressive decrease in propagation velocity. Statistical analysis revealed a transition from approximately Gaussian pre-flare intensity distributions to increasingly right-skewed distributions during the eruption, with corresponding increases in variability, skewness,and kurtosis.