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| − | Supernovae are more [[Energy|energetic]] than a [[nova]]. ''Nova'' means "new" in [[Latin language|Latin]], referring to what appears to be a very bright new star shining in the [[celestial sphere]]; the prefix "super-" distinguishes supernovae from ordinary novae which are far less luminous. The word ''supernova'' was coined by [[Walter Baade]] and [[Fritz Zwicky]] in 1931.<ref name=baas33_1330/> It is pronounced {{IPAc-en||ˌ|s|uː|p|ə|ˈ|n|oʊ|v|ə}} with the plural '''''supernovae''''' {{IPAc-en|ˌ|s|uː|p|ə|ˈ|n|oʊ|v|iː}} or '''''supernovas''''' (abbreviated '''''SN''''', plural '''''SNe''''' after "supernovae").
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| − | Supernovae can be triggered in one of two ways: by the sudden reignition of [[nuclear fusion]] in a [[Compact star|degenerate star]]; or by the [[gravitational collapse]] of the core of a massive star. A degenerate [[white dwarf]] may accumulate sufficient material from a [[Binary star|companion]], either through [[Accretion (astrophysics)|accretion]] or via a merger, to raise its core temperature, [[Carbon detonation|ignite]] [[Carbon burning process|carbon fusion]], and trigger [[Thermal runaway|runaway]] nuclear fusion, completely disrupting the star. The core of a [[stellar evolution#Massive stars|massive star]] may undergo sudden [[gravitational collapse]], releasing [[gravitational potential energy]] that can create a supernova explosion.
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| − | Although no supernova has been observed in the [[Milky Way]] since Kepler's Star of 1604 ([[SN 1604]]), supernova remnants indicate that on average the event occurs about three times every century in the Milky Way.
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