![]() Since most of the matter in the core is converted into neutrons, they are known as neutron stars. The positive charge of the proton and the negative charge of the electron cancel each other out, and the resulting particle becomes a neutron. Since the electrons were stripped from their atoms during the core collapse, most of the protons in the star end up absorbing an electron. Neutron StarsĪlthough the blast from a supernova sometimes destroys a star completely, usually the core of the star remains. As with planetary nebulae, supernovae blast heavy elements into the interstellar medium that will eventually form into new stars and planets. Once a supernova has subsided, the dust and gas forms a large nebula where new stars can form. Thus, supernovae are responsible for most of the elements heavier than iron, such as tin, gold and lead. The tremendous amounts of energy released in a supernova are enough to fuse additional particles into the nuclei of heavy elements such as iron and nickel. The massive amounts of radiation released during a supernova makes them so bright that they are generally some of the brightest objects in the sky, though they fade in a number of weeks. This collapse creates a massive shock wave that rips the star apart in a massive explosion called a supernova. The atoms in the core collapse, leaving nothing but their atomic nuclei. A supergiant's core is so massive, that even pressure exerted by the electrons can't support the force of gravity. When a supergiant can no longer maintain equilibrium, it undergoes a sudden catestrophic collapse. Like Red Dwarfs, however, their lifespan far exceeds the age of the universe, which means that no White Dwarfs are old enough to have stopped shining. Fusion has already ceased in White Dwarfs, which means that they will slowly cool until they no longer give off light. Since white dwarfs are created from the cores of red giants, they are composed of elements like carbon, oxygen and neon. Although they may have about as much mass as our sun, even after ejecting most of their mass as a planetary nebula, they are compressed to a tiny ball about the size of the earth. White dwarfs are very hot and bright, but very small. Once gravity has collapsed the atoms of the star so close together that their electrons can't get any closer, this pressure from the electrons is enough to keep the star from collapsing further. This pressure occurs because subatomic particles like electrons don't like to share the same space. In a white dwarf, the force of gravity compressing the star is balanced by a electron degeneracy pressure. The exposed core of a Red Giant that is left behind after the formation of a planetary nebula is known as a white dwarf. The more of these elements a star pulls in as it is forming, the more likely that the star will also form planets. More heavy elements in the interstellar medium means more heavy elements being pulled into future protostars. These elements are blown back into the interstellar medium, enriching it with more heavy elements. Helium, carbon and small amounts of other elements can also be found in them. Because of the intense fusion reactions that take place inside stars, planetary nebulae tend to be made up of more than just hydrogen. ![]() These outer layers become known as a planetary nebula. When a Red Giant dies, the heat and pressure from its core ejects the outer layers of the star into space. ![]() Manny of these stellar remnants have unusual properties, making them some of the most interesting and exciting objects for astronomers to study. ![]() A number of the objects we see in the sky are not stars, but the remains of stars that have died. ![]()
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