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Currently, our Sun is a content, middle-aged main sequence star steadily fusing hydrogen atoms into helium atoms and releasing radiation in many of the wavelengths making up the electromagnetic spectrum. So what happens between now and when the Sun runs out of hydrogen? And what happens after that? Before we can answer these questions, we need to take a look at what goes on within a star’s hot interior and how that energy reaches the surface of the Sun and then onward out into the surrounding space.