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Supernovas are among the most energetic events in the universe and result in the complete disruption of stars at the end of their lives. Originally, the distinction between Type I and Type II supernovas was based solely on the presence or absence of hydrogen atoms (hydrogen lines). Supernovas without hydrogen lines were called Type I, while those with hydrogen lines were Type II. Subsequent analysis of many of these events revealed that this empirical classification schema instead reflected two different mechanisms for the supernova explosion.
Type I supernovas happen in binary stars — two stars that orbit closely each other — when one of the two binary stars is a small, dense, white dwarf star. If the companion star ranges too close to the white dwarf that it is orbiting, the white dwarf’s gravitational pull will draw matter from the other star. When the white dwarf acquires enough matter to become at least 1.4 times as big as the Sun, it collapses and explodes in a supernova.
Type II supernovas occur when a star, much more massive than the Sun, ends its life. When such a star begins burning out, the core of the star quickly collapses releasing amazing energy in the form of neutrinos, a kind of particle smaller than even an atom. Electromagnetic radiation — energy that is electric and magnetic— causes the star to explode in a supernova. Whereas Type I supernovas typically destroy their parent stars, Type II explosions usually leave behind the stellar core.
The classification schema regarding the mechanism for supernova explosions helps to more succinctly answer the question: Is the Sun in danger of becoming a supernova? Neither does our Sun have a companion star orbiting it nor does our Sun have the mass necessary to become a supernova. Furthermore, it will be another billion years until the Sun runs out of fuel and swells into a red giant star before going into a white dwarf form.