The Solar atmosphere is a subject of intensive study due to a scientifically popular anomaly, which is that the Sun’s visible surface, the photosphere, is a couple thousand Kelvin in temperature while the atmosphere (Solar corona in particular) is a couple million. The reason why it may be is still a subject of debate and studying the temperature distribution of the solar atmosphere will prove to be helpful for further investigation. The project involves the use of EUV solar spectroscopy to study the structure of the coronal active regions and their inferred properties of the plasma. Under the affiliation with the University of Glasgow, I aim to find the temperature distribution gradient of the solar corona in my specific region of study of the solar disk. This information should provide an insight into the behavior of the Solar surface as is intended.