Calculation and Comparison of Velocities of Magnetic Loops on Sun’s Surface Using Ions at Different Temperatures

It has been found that the surface of the Sun (the photosphere) has a lower temperature than the outer atmosphere (corona). As energy is generated in the 15-million-degree core due to nuclear fusion, it flows outwards to the photosphere and the corona. However, while the temperature of the photosphere is 5000 Kelvin, the temperature of the corona can be over 10^6 Kelvin. Currently, the heating mechanism that causes this drastic change in temperature is unknown. The answer to this seems to be in the magnetic loops that form below the photosphere and rise to the corona. The study of these magnetic loops on the surface can pave the way for a better understanding of the mechanisms that heat the outer atmosphere of the Sun. In addition, it can help provide insight into predicting solar flares and other solar activity. Specifically, the aim of our research is to produce velocity measurements that allow for a comparison with the results of computer models that employ different heating methods. Our research is based on EIS data from the Hinode spacecraft. Using Python and Python packages, we plotted points on the ultraviolet image of the Sun to identify a magnetic loop. These points were analyzed for different ions with different spectral lines. We fit each spectral line with a Gaussian function; from the resulting parameters, we calculated the velocities using the Doppler effect. Based on the calculated velocities, we presented velocity graphs as a function of ions of different temperatures.