Science, Tech, Math › Science Supernovae: Catastrophic Explosions of Giant Stars Share Flipboard Email Print This is what's left when a massive star explodes as a supernova. The Hubble Space Telescope captured this image of the Crab Nebula, a supernova remnant more than 6,000 light-years away from Earth. NASA Science Astronomy Stars, Planets, and Galaxies An Introduction to Astronomy Important Astronomers Solar System Space Exploration Chemistry Biology Physics Geology Weather & Climate By John P. Millis, Ph.D Professor of Physics and Astronomy Ph.D., Physics and Astronomy, Purdue University B.S., Physics, Purdue University our editorial process John P. Millis, Ph.D Updated January 10, 2020 Supernovae are the most destructive things that can happen to stars more massive than the Sun. When these catastrophic explosions occur, they release enough light to outshine the galaxy where the star existed. That's a lot of energy being released in the form of visible light and other radiation! They can also blow the star apart. There are two known types of supernovae. Each type has its own particular characteristics and dynamics. Let's take a look at what supernovae are and how they come about in the galaxy. Type I Supernovae To understand a supernova, it's important to know a few things about stars. They spend most of their lives going through a period of activity called being on the main sequence. It begins when nuclear fusion ignites in the stellar core. It ends when the star has exhausted the hydrogen needed to sustain that fusion and begins fusing heavier elements. Once a star leaves the main sequence, its mass determines what happens next. For type I supernovae, which occur in binary star systems, stars that are about 1.4 times the mass of our Sun go through several phases. They move from fusing hydrogen to fusing helium. At that point, the core of the star is not at a high enough temperature to fuse carbon, and so it enters a super red-giant phase. The outer envelope of the star slowly dissipates into the surrounding medium and leaves a white dwarf (the remnant carbon/oxygen core of the original star) at the center of a planetary nebula. Basically, the white dwarf has a strong gravitational pull that attracts material from its companion. That "star stuff" collects into a disk around the white dwarf, known as an accretion disk. As the material builds up, it falls onto the star. That increases the mass of the white dwarf. Eventually, as the mass increases to about 1.38 times the mass of our Sun, the star erupts in a violent explosion known as a Type I supernova. There are some variations on this theme, such as the merger of two white dwarfs (instead of the accretion of material from a main-sequence star onto its dwarf companion). Type II Supernovae Unlike Type I supernovae, Type II supernovae happen to very massive stars. When one of these monsters reaches the end of its life, things go quickly. Whereas stars like our Sun won't have enough energy in their cores to sustain fusion past carbon, larger stars (more than eight times the mass of our Sun) will eventually fuse elements all the way up to iron in the core. Iron fusion takes more energy than the star has available. Once such a star tries to fuse iron, a catastrophic end is inevitable. Once the fusion ceases in the core, the core will contract due to the immense gravity and the outer part of the star "falls" onto the core and rebounds to create a massive explosion. Depending on the mass of the core, it will either become a neutron star or black hole. If the mass of the core is between 1.4 and 3.0 times the mass of the Sun, the core will become a neutron star. This is simply a big ball of neutrons, packed very tightly together by gravity. It happens when the core contracts and undergoes a process known as neutronization. That's where the protons in the core collide with very high-energy electrons to create neutrons. As this happens the core stiffens and sends shock waves through the material that is falling onto the core. The outer material of the star is then driven out into the surrounding medium creating the supernova. All of this happens very quickly. Creating a Stellar Black Hole Should the mass of the dying star's core be greater than three to five times the mass of the Sun, then the core will not be able to support its own immense gravity and will collapse into a black hole. This process will also create shock waves that drive material into the surrounding medium, creating the same kind of supernova as the type of explosion that creates a neutron star. In either case, whether a neutron star or black hole is created, the core is left behind as a remnant of the explosion. The rest of the star is blown out to space, seeding nearby space (and nebulae) with heavy elements needed for the formation of other stars and planets. Key Takeaways Supernovae come in two flavors: Type 1 and Type II (with subtypes such as Ia and IIa). A supernova explosion often blows a star apart, leaving behind a massive core.Some supernova explosions result in the creation of stellar-mass black holes. Stars like the Sun do NOT die as supernovae. Edited and updated by Carolyn Collins Petersen.