## 1 Introduction  
The sun, being the star closest to us, plays a significant role in our solar system, and phenomena such as coronal mass ejections (CMEs) during solar activities have widespread effects on the Earth. Intense solar activity could lead to catastrophic weather events on our planet, pose risks to space operations, and may even threaten human lives [1]. Therefore, monitoring and researching solar coronal activities is of great significance to humanity [2]. The Atmospheric Imaging Assembly (SDO/AIA) of the Solar Dynamics Observatory provides critical information for human observation of solar activities. The Coronal Mass Ejection on 13 June 2010, and its associated extreme ultraviolet wave, were studied using high-resolution core channel data of 193 A and 211 A from the Atmospheric Imaging Assembly [3,4] on board the Solar Dynamics Observatory [5]. The 171 A filter of AIA is particularly suitable for observing plume-like structures and large coronal loops, features that are often found in the corona's quiescent areas and regions with weaker magnetic fields. The 193 A filter of AIA is specifically appropriate for observing coronal structures within active regions, such as active coronal loops and solar flares. [PERSON] et al. (2013) [6] used AIA's 193 and 211 channels to validate the fundamental physical mechanisms of the prevalent flare models, providing visual evidence of magnetic reconnection generating solar flares. [PERSON] et al. (2016) [7] demonstrated a new role in the solar eruptions' reconnection through AIA's 131, 171, and 304 bands: the release of magnetic torsion. [PERSON] et al. (2021) [8] compared AIA with high-resolution EUV telescopes and found that \"campfires\"(Small-scale localized bright regions, also known as 'campfires,' appear in the quiet areas of the Sun, with lengths ranging from 400 to 4000 km and durations from 10 s to 200 s) are essentially coronal in nature, originating from the magnetic flux concentrations of the chromospheric network. Higher resolution data also provide a more comprehensive perspective for the observation of solar activities. The High-resolution Coronal Imager (Hi-C) captured extremely clear coronal images in 193 angstrom and 172 angstrom wavelengths, respectively, in 2012 and 2018. These images had a resolution of at least 0.47 arcseconds, providing an unprecedented opportunity to study the mass and energy coupling between the chromosphere and the corona. [PERSON] et al. (2013) [9] confirmed the existence of various heating mechanisms in the solar outer atmosphere, or corona, through the solar coronal images captured by Hi-C. [PERSON] et al. (2014) [10] found evidence of small-scale extreme ultraviolet (EUV) heating events at the bases of coronal loops in high-definition images. [PERSON] (2015) [11] revealed detailed information that helps us understand the dynamics of the magnetic field, fine structures, and flare energy release. [PERSON] (2017) [12] observed that the size, motion, and temporal evolution of coronal loop features are associated with photospheric motions, indicating that they are closely connected to the photospheric magnetic field. [PERSON] et al. (2020) [13] discovered that current density is proportional to magnetic field strength and emphasized the importance of establishing a permanent solar observatory facility with high resolution similar to Hi-C. This motivates us to work on improving the quality of SDO/AIA images to match the resolution of Hi-C and to provide higher temporal resolution coronal images for solar imagery research. This has inspired us to endeavor to enhance the quality of SDO/AIA images to achieve the same resolution as that of Hi-C, and to furnish solar image research with coronal images of higher temporal resolution. The resolution of observed solar images is constrained by the capabilities of the instruments. Even with the most advanced instruments available today, it is challenging to achieve the high resolution that theoretical solar physicists aspire to.