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Interesting question.This is what Wikipedia had to say.Near-Earth supernovaFrom Wikipedia, the free encyclopediaJump to navigation Jump to searchMain article: History of supernova observationThe Crab Nebula is a pulsar wind nebula associated with the 1054 supernova. It is located about 6,500 light-years from the Earth.[1]A near-Earth supernova is an explosion resulting from the death of a star that occurs close enough to the Earth (roughly less than 10 to 300 parsecs (30 to 1000 light-years) away[2]) to have noticeable effects on Earth's biosphere.Historically, each near-Earth supernova explosion has been associated with a global warming of around 3–4 °C. An estimated 20 supernovae explosions have happened within 300 pc of the Earth over the last 11 million years. Type II supernovae explosions are expected to occur in active star-forming regions, with 12 such OB associations being located within 650 pc of the Earth. At present, there are six near-Earth supernova candidates within 300 pc.[3]Contents1 Effects on Earth2 Risk by supernova type3 Past events4 See also5 Footnotes6 ReferencesEffects on EarthOn average, a supernova explosion occurs within 10 parsecs (33 light-years) of the Earth every 240 million years.[a]Gamma rays are responsible for most of the adverse effects a supernova can have on a living terrestrial planet. In Earth's case, gamma rays induce radiolysis of diatomicN2 and O2 in the upper atmosphere, converting molecular nitrogen and oxygen into nitrogen oxides, depleting the ozone layer enough to expose the surface to harmful solar and cosmic radiation (mainly ultra-violet). Phytoplankton and reef communities would be particularly affected, which could severely deplete the base of the marine food chain.[4][5]Odenwald[6]discusses the possible effects of a Betelgeuse supernova on the Earth and on human space travel, especially the effects of the stream of charged particles that would reach the Earth circa 100,000 years later than the initial light and other electromagnetic radiation produced by the explosion.Risk by supernova typeCandidates within 300 pc[3]Star DesignationDistance(pc)Mass(M☉)IK Pegasi461.65/1.15Spica8010.25/7.0Alpha Lupi14110.1Antares16912.4/10Betelgeuse1977.7–20Rigel26418Speculation as to the effects of a nearby supernova on Earth often focuses on large stars as Type II supernova candidates. Several prominent stars within a few hundred light years of the Sun are candidates for becoming supernovae in as little as a millennium. Although they would be spectacular to look at, were these "predictable" supernovae to occur, they are thought to have little potential to affect Earth.It is estimated that a Type II supernova closer than eight parsecs (26 light-years) would destroy more than half of the Earth's ozone layer.[7]Such estimates are based on atmospheric modeling and the measured radiation flux from SN 1987A, a Type II supernova in the Large Magellanic Cloud. Estimates of the rate of supernova occurrence within 10 parsecs of the Earth vary from 0.05–0.5 per Ga[5]to 10 per Ga.[8]Several studies assume that supernovae are concentrated in the spiral arms of the galaxy, and that supernova explosions near the Sun usually occur during the ~10 million years that the Sun takes to pass through one of these regions.[7]Examples of relatively near supernovae are the Vela Supernova Remnant (~800 ly, ~12,000 years ago) and Geminga (~550 ly, ~300,000 years ago).Type Ia supernovae are thought to be potentially the most dangerous if they occur close enough to the Earth. Because Type Ia supernovae arise from dim, common white dwarf stars, it is likely that a supernova that could affect the Earth will occur unpredictably and take place in a star system that is not well studied. The closest known candidate is IK Pegasi.[9]It is currently estimated, however, that by the time it could become a threat, its velocity in relation to the Solar System would have carried IK Pegasi to a safe distance.[7]Past eventsEvidence from daughter products of short-lived radioactive isotopes shows that a nearby supernova helped determine the composition of the Solar System 4.5 billion years ago, and may even have triggered the formation of this system.[10]Supernova production of heavy elements over astronomic periods of time ultimately made the chemistry of life on Earth possible.Past supernovae might be detectable on Earth in the form of metal isotope signatures in rock strata. Subsequently, iron-60 enrichment has been reported in deep-sea rock of the Pacific Ocean by researchers from the Technical University of Munich.[11][12][13]Twenty-three atoms of this iron isotope were found in the top 2 cm of crust (this layer corresponds to times from 13.4 to 0 million years ago).[13]It is estimated that the supernova must have occurred in the last 5 million years or else it would have had to happen very close to the solar system to account for so much iron-60 still being here. A supernova occurring so close would have probably caused a mass extinction, which did not happen in that time frame.[14]The quantity of iron seems to indicate that the supernova was less than 30 parsecs away. On the other hand, the authors estimate the frequency of supernovae at a distance less than D (for reasonably small D) as around (D/10 pc)3per Ga, which gives a probability of only around 5% for a supernova within 30 pc in the last 5 million years. They point out that the probability may be higher because the Solar System is entering the Orion Arm of the Milky Way.Gamma ray bursts from "dangerously close" supernova explosions occur two or more times per billion years, and this has been proposed as the cause of the end Ordovician extinction, which resulted in the death of nearly 60% of the oceanic life on Earth.[15]In 1998 a supernova remnant, RX J0852.0-4622, was found in front (apparently) of the larger Vela Supernova Remnant.[16]Gamma rays from the decay of titanium-44 (half-life about 60 years) were independently discovered emanating from it,[17]showing that it must have exploded fairly recently (perhaps around 1200 CE), but there is no historical record of it. The flux of gamma rays and x-rays indicates that the supernova was relatively close to us (perhaps 200 parsecs or 660 ly). If so, this is an unexpected event because supernovae less than 200 parsecs away are estimated to occur less than once per 100,000 years.[13]See alsoList of supernova candidatesFootnotesSince a radius of 100 light years contains approximately 27.8 times as much volume as one of 33 light years, a supernova should occur within a radius of 100 light years from Earth approximately once every 8.6 million years. A supernova would occur within a radius of 200 light years approximately once every million years, within 500 light years every 69,000 years, and within 1,000 light years roughly every 8,625 years.[original research?]ReferencesKaplan, D. L.; Chatterjee, S.; Gaensler, B. M.; Anderson, J. (2008). "A Precise Proper Motion for the Crab Pulsar, and the Difficulty of Testing Spin-Kick Alignment for Young Neutron Stars". The Astrophysical Journal. 677 (2): 1201–1215. arXiv:0801.1142. Bibcode:2008ApJ...677.1201K. doi:10.1086/529026.Joshua Sokol (Jan 14, 2016). "What If History's Brightest Supernova Exploded In Earth's Backyard?". The Atlantic.Firestone, R. B. (July 2014). "Observation of 23 Supernovae That Exploded <300 pc from Earth during the past 300 kyr". The Astrophysical Journal. 789 (1): 11. Bibcode:2014ApJ...789...29F. doi:10.1088/0004-637X/789/1/29. 29.Ellis, J.; Schramm, D. N. (1993). "Could a nearby supernova explosion have caused a mass extinction?". Proceedings of the National Academy of Sciences of the United States of America. 92 (1): 235–8. arXiv:hep-ph/9303206. Bibcode:1993hep.ph....3206E. doi:10.1073/pnas.92.1.235. PMC 42852. PMID 11607506.Whitten, R. C.; Borucki, W. J.; Wolfe, J. H.; Cuzzi, J. (1976). "Effect of nearby supernova explosions on atmospheric ozone". Nature. 263 (5576): 398–400. Bibcode:1976Natur.263..398W. doi:10.1038/263398a0."The Betelgeuse Supernova". 2015-02-02.Gehrels, N.; et al. (2003). "Ozone Depletion from Nearby Supernovae". The Astrophysical Journal. 585 (2): 1169–1176. arXiv:astro-ph/0211361. Bibcode:2003ApJ...585.1169G. doi:10.1086/346127.Clark, D. H.; McCrea, W. H.; Stephenson, F. R. (1977). "Frequency of nearby supernovae and climactic and biological catastrophes". Nature. 265 (5592): 318–319. Bibcode:1977Natur.265..318C. doi:10.1038/265318a0.Garlick, M. (March 2007). "The Supernova Menace". Sky & Telescope. 113 (3): 3.26. Bibcode:2007S&T...113c..26G.Taylor, G. J. (2003-05-21). "Triggering the Formation of the Solar System". Planetary Science Research. Retrieved 2006-10-20.Staff (Fall 2005). "Researchers Detect 'Near Miss' Supernova Explosion". University of Illinois College of Liberal Arts and Sciences. p. 17. Archived from the original on 2006-09-01. Retrieved 2007-02-01.Knie, K.; et al. (2004). "60Fe Anomaly in a Deep-Sea Manganese Crust and Implications for a Nearby Supernova Source". Physical Review Letters. 93 (17): 171103–171106. Bibcode:2004PhRvL..93q1103K. doi:10.1103/PhysRevLett.93.171103. PMID 15525065.Fields, B. D.; Ellis, J. (1999). "On Deep-Ocean Fe-60 as a Fossil of a Near-Earth Supernova". New Astronomy. 4 (6): 419–430. arXiv:astro-ph/9811457. Bibcode:1999NewA....4..419F. doi:10.1016/S1384-1076(99)00034-2.Fields & Ellis, p. 10Melott, A.; et al. (2004). "Did a gamma-ray burst initiate the late Ordovician mass extinction?". International Journal of Astrobiology. 3 (2): 55–61. arXiv:astro-ph/0309415. Bibcode:2004IJAsB...3...55M. doi:10.1017/S1473550404001910.Aschenbach, B. (1998). "Discovery of a young nearby supernova remnant". Nature. 396 (6707): 141–142. Bibcode:1998Natur.396..141A. doi:10.1038/24103.Iyudin, A. F.; et al. (1998). "Emission from 44Ti associated with a previously unknown Galactic supernova". Nature. 396 (6707): 142–144. Bibcode:1998Natur.396..142I. doi:10.1038/24106.vteSupernovaeClassesType IaType Ib and IcType II (IIP, IIL, IIn, and IIb)Physics ofCalcium-rich supernovaeCarbon detonationPair-instability supernovaPhillips relationshipP-nucleiP-processR-processSupernova nucleosynthesisSupernova neutrinosRelatedSupernova impostor Pulsational pair-instability supernovaFoeGamma-ray burstFailed supernovaHypernovaKilonovaNovaSymbiotic novaLuminous red novaNear-Earth supernovaPulsar kickQuark-novaProgenitorsHypergiant YellowLuminous blue variableSupergiant Blue Red YellowWhite dwarf Related linksWolf–Rayet starRemnantsSupernova remnant Pulsar wind nebulaNeutron star Pulsar Magnetar Related linksStellar black hole Related linksCompact star Quark star Exotic starZombie starLocal BubbleSuperbubble Orion–EridanusDiscoveryGuest starHistory of supernova observationTimeline of white dwarfs, neutron stars, and supernovaeListsCandidatesNotableMassive starsMost distantRemnantsIn fictionNotableBarnard's LoopCassiopeia ACrab Crab NebulaiPTF14hlsTycho'sKepler'sSN 1987ASN 185SN 1006SN 2003fgRemnant G1.9+0.3SN 2007biSN 2011feSN 2014JSN RefsdalVela RemnantResearchASAS-SNCalán/Tololo SurveyHigh-Z Supernova Search TeamKatzman Automatic Imaging TelescopeMonte Agliale Supernovae and Asteroid SurveyNearby Supernova FactorySloan Supernova SurveySupernova/Acceleration ProbeSupernova Cosmology ProjectSupernova Early Warning SystemSupernova Legacy SurveyTexas Supernova SearchBook:SupernovaeCategory:SupernovaeCommons:SupernovaeCategories:Natural hazardsEarthSupernovaeSpace hazardsDoomsday scenariosNavigation menuNot logged inTalkContributionsCreate accountLog inArticleTalkReadEditView historySearchMain pageContentsFeatured contentCurrent eventsRandom articleDonate to WikipediaWikipedia storeInteractionHelpAbout WikipediaCommunity portalRecent changesContact pageToolsWhat links hereRelated changesUpload fileSpecial pagesPermanent linkPage informationWikidata itemCite this pagePrint/exportCreate a bookDownload as PDFPrintable versionLanguagesالعربية한국어日本語RomânăРусскийTürkçeУкраїнська中文Edit linksThis page was last edited on 11 April 2019, at 04:24 (UTC).Text is available under the Creative Commons Attribution-ShareAlike License; additional terms may apply. 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