![]() ![]() Only a tiny fraction of the 100 billion stars in a typical galaxy have the capacity to become a supernova, being restricted to those having high mass and rare kinds of binary stars containing white dwarfs. Main article: History of supernova observationĬompared to a star's entire history, the visual appearance of a supernova is very brief, sometimes spanning several months, so that the chances of observing one with the naked eye is roughly once in a lifetime. Its first use in a journal article came the following year in a publication by Knut Lundmark, who may have coined it independently. ![]() The word supernova was coined by Walter Baade and Fritz Zwicky, who began using it in astrophysics lectures in 1931. Adding the prefix "super-" distinguishes supernovae from ordinary novae, which are far less luminous. It is derived from the Latin word nova, meaning "new", which refers to what appears to be a temporary new bright star. The word supernova has the plural form supernovae /- v iː/ or supernovas and is often abbreviated as SN or SNe. They might also produce gravitational waves, though thus far gravitational waves have been detected only from the mergers of black holes and neutron stars. Supernovae are a major source of cosmic rays. The expanding shock waves of supernovae can trigger the formation of new stars. Supernovae are a major source of elements in the interstellar medium from oxygen to rubidium. This drives an expanding shock wave into the surrounding interstellar medium, sweeping up an expanding shell of gas and dust observed as a supernova remnant. Supernovae can expel several solar masses of material at velocities up to several percent of the speed of light. In the case of a massive star's sudden implosion, the core of a massive star will undergo sudden collapse once it is unable to produce sufficient energy from fusion to counteract the star's own gravity, which must happen once the star begins fusing iron, but may happen during an earlier stage of metal fusion.Possible causes are an accumulation of material from a binary companion through accretion, or by a stellar merger. In the re-ignition of a white dwarf, the object's temperature is raised enough to trigger runaway nuclear fusion, completely disrupting the star.Theoretical studies indicate that most supernovae are triggered by one of two basic mechanisms: the sudden re-ignition of nuclear fusion in a white dwarf, or the sudden gravitational collapse of a massive star's core. The most recent naked-eye supernova was SN 1987A, which was the explosion of a blue supergiant star in the Large Magellanic Cloud, a satellite of the Milky Way. A supernova in the Milky Way would almost certainly be observable through modern astronomical telescopes. The remnants of more recent supernovae have been found, and observations of supernovae in other galaxies suggest they occur in the Milky Way on average about three times every century. ![]() The last supernova directly observed in the Milky Way was Kepler's Supernova in 1604, appearing not long after Tycho's Supernova in 1572, both of which were visible to the naked eye. The peak optical luminosity of a supernova can be comparable to that of an entire galaxy before fading over several weeks or months. The original object, called the progenitor, either collapses to a neutron star or black hole, or is completely destroyed to form a diffuse nebula. A supernova occurs during the last evolutionary stages of a massive star or when a white dwarf is triggered into runaway nuclear fusion. SN 1994D (bright spot on the lower left), a type Ia supernova within its host galaxy, NGC 4526Ī supernova ( PL: supernovae or supernovas) is a powerful and luminous explosion of a star. For other uses, see Supernova (disambiguation). ![]()
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