"\u0645\u0633\u062A\u0639\u0631 \u0623\u0639\u0638\u0645"@ar . . . . . . . . . . . . . "\u8D85\u65B0\u661F"@ja . . . "Supernovao estas giganta steleksplodo, per kiu la tuta materialo de pezega stelo (10 foje a\u016D pli ol la suna maso), escepte de \u011Dia centra kerno, di\u015Djeti\u011Das tra la interstelan spacon. La heleco de tia eksplodo estas tiel, ke foje eblas vidi \u011Din per nuda okulo en la \u0109ielo. \n* Resta\u0135o de la Keplera supernovao, kiu eksplodis la 9-an de oktobro 1604. \n* Resta\u0135oj de supernovao 1987A en Granda Magelana Nubo (en centro). Helaj blankaj objektoj maldekstre supre kaj dekstre malsupre estas la aliaj steloj. \n* Dependo de heleco de supernovao de tempo por specoj de supernovaoj II-P kaj II-L. \n* Bildo de SN 1006 en rentgenaj radioj"@eo . . . . . 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"Term\u00EDn supernova nebo v\u00FDbuch supernovy (exploze supernovy) se v astronomii vztahuje k n\u011Bkolika typ\u016Fm hv\u011Bzdn\u00FDch exploz\u00ED, kter\u00FDmi vznikaj\u00ED extr\u00E9mn\u011B jasn\u00E9 objekty slo\u017Een\u00E9 z plazmatu, jejich\u017E jasnost nakonec v pr\u016Fb\u011Bhu t\u00FDdn\u016F \u010Di m\u011Bs\u00EDc\u016F op\u011Bt o mnoho \u0159\u00E1d\u016F kles\u00E1. K explozi vedou dv\u011B mo\u017En\u00E9 cesty: - jedn\u00E1 se o masivn\u00ED hv\u011Bzdu, kter\u00E1 ve sv\u00E9m j\u00E1d\u0159e syntetizovala takov\u00E9 mno\u017Estv\u00ED \u017Eeleza nezp\u016Fsobil\u00E9ho jadern\u00E9 f\u00FAze, \u017Ee se gravita\u010Dn\u011B zhrout\u00ED pod silou sv\u00E9 vlastn\u00ED gravitace, jej\u00ED\u017E p\u016Fsoben\u00ED ji\u017E nevyrovn\u00E1 utlumen\u00E1 f\u00FAzn\u00ED reakce."@cs . "Term\u00EDn supernova nebo v\u00FDbuch supernovy (exploze supernovy) se v astronomii vztahuje k n\u011Bkolika typ\u016Fm hv\u011Bzdn\u00FDch exploz\u00ED, kter\u00FDmi vznikaj\u00ED extr\u00E9mn\u011B jasn\u00E9 objekty slo\u017Een\u00E9 z plazmatu, jejich\u017E jasnost nakonec v pr\u016Fb\u011Bhu t\u00FDdn\u016F \u010Di m\u011Bs\u00EDc\u016F op\u011Bt o mnoho \u0159\u00E1d\u016F kles\u00E1. K explozi vedou dv\u011B mo\u017En\u00E9 cesty: - jedn\u00E1 se o masivn\u00ED hv\u011Bzdu, kter\u00E1 ve sv\u00E9m j\u00E1d\u0159e syntetizovala takov\u00E9 mno\u017Estv\u00ED \u017Eeleza nezp\u016Fsobil\u00E9ho jadern\u00E9 f\u00FAze, \u017Ee se gravita\u010Dn\u011B zhrout\u00ED pod silou sv\u00E9 vlastn\u00ED gravitace, jej\u00ED\u017E p\u016Fsoben\u00ED ji\u017E nevyrovn\u00E1 utlumen\u00E1 f\u00FAzn\u00ED reakce. - jedn\u00E1 se o b\u00EDl\u00E9ho trpasl\u00EDka, kter\u00FD nahromadil materi\u00E1l od sv\u00E9ho hv\u011Bzdn\u00E9ho pr\u016Fvodce, dos\u00E1hl Chandrasekharovy meze a prod\u011Blal termonukle\u00E1rn\u00ED explozi. V obou p\u0159\u00EDpadech v\u00FDsledn\u00FD v\u00FDbuch supernovy rozmet\u00E1 obrovskou silou v\u011Bt\u0161inu nebo v\u0161echnu hmotu hv\u011Bzdy. Exploze vytv\u00E1\u0159\u00ED r\u00E1zovou vlnu, kter\u00E1 se \u0161\u00ED\u0159\u00ED do okoln\u00EDho prostoru, interaguje se zbytky supernovy a mezihv\u011Bzdnou hmotou. Nejzn\u00E1m\u011Bj\u0161\u00EDm p\u0159\u00EDkladem tohoto procesu jsou zbytky SN 1604, kter\u00E9 lze vid\u011Bt na obr\u00E1zku. Exploze supernov jsou jedn\u00EDm ze zdroj\u016F v\u0161ech prvk\u016F t\u011B\u017E\u0161\u00EDch ne\u017E \u017Eelezo ve vesm\u00EDru. Dal\u0161\u00EDm zdrojem jsou kolize neutronov\u00FDch hv\u011Bzd. Nap\u0159\u00EDklad v\u0161echen zinek, zlato a uran byly syntetizov\u00E1ny p\u0159i explozi supernov nebo koliz\u00ED neutronov\u00FDch hv\u011Bzd p\u0159ed miliardami let. Supernovy vn\u00E1\u0161ej\u00ED do mezihv\u011Bzdn\u00E9 hmoty t\u011B\u017Ek\u00E9 prvky a obohacuj\u00ED tak molekul\u00E1rn\u00ED mra\u010Dna, kter\u00E1 jsou d\u011Bji\u0161t\u011Bm tvorby nov\u00FDch hv\u011Bzd. \u010Cinnost supernov v\u00FDznamn\u011B ovlivnila slo\u017Een\u00ED slune\u010Dn\u00ED soustavy a umo\u017Enila tak nakonec \u017Eivot na Zemi, jak ho zn\u00E1me. V\u00FDbuch supernovy je prov\u00E1zen obrovsk\u00FDmi teplotami a za jist\u00FDch podm\u00EDnek mohou f\u00FAzn\u00ED reakce b\u011Bhem vrcholn\u00E9 f\u00E1ze vyprodukovat n\u011Bkter\u00E9 z nejt\u011B\u017E\u0161\u00EDch prvk\u016F, jako je kalifornium. Podstatu jevu i samotn\u00FD n\u00E1zev \u201Esupernova\u201D poprv\u00E9 p\u0159edstavili ve\u0159ejnosti Fritz Zwicky a Walter Baade na p\u0159edn\u00E1\u0161ce na Stanfordov\u011B univerzit\u011B 15. prosince 1933. P\u016Fvodn\u00ED v\u00FDraz nova (latinsky (stella) nova, \u201Enov\u00E1 (hv\u011Bzda)\u201C) ozna\u010Doval obdobn\u00FD jev, kter\u00FD byl pozorov\u00E1n jako nov\u011B vznikl\u00E1 jasn\u00E1 a kr\u00E1tce sv\u00EDt\u00EDc\u00ED hv\u011Bzda na nebesk\u00E9 sf\u00E9\u0159e. Za\u017Eit\u00FD term\u00EDn nova se nezm\u011Bnil ani po zji\u0161t\u011Bn\u00ED, \u017Ee se nejedn\u00E1 o novou hv\u011Bzdu, ale o f\u00E1zi ve v\u00FDvoji hv\u011Bzdy na konci jej\u00EDho \u017Eivota. P\u0159edpona \u201Esuper\u201C odr\u00E1\u017E\u00ED skute\u010Dnost, \u017Ee p\u0159i v\u00FDbuchu supernovy se uvol\u0148uje mnohem v\u00EDce energie; p\u0159edpokl\u00E1dan\u00E9 nejv\u011Bt\u0161\u00ED supernovy se naz\u00FDvaj\u00ED hypernovy."@cs . . . 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\u0647\u0648 1.4 \u0643\u062A\u0644\u0629 \u0634\u0645\u0633\u064A\u0629 \u0641\u0625\u0630\u0627 \u0643\u0627\u0646\u062A \u0643\u062A\u0644\u0629 \u0627\u0644\u0646\u062C\u0645 \u0623\u0643\u0628\u0631 \u0645\u0646 1.4 \u0643\u062A\u0644\u0629 \u0634\u0645\u0633\u064A\u0629 \u0641\u0625\u0646 \u0627\u0644\u0646\u062C\u0645 \u064A\u0645\u0631 \u0628\u0645\u0631\u062D\u0644\u0629 \u0627\u0644\u0645\u0633\u062A\u0639\u0631 \u0627\u0644\u0623\u0639\u0638\u0645 \u0648\u064A\u062A\u0628\u0642\u0649 \u0645\u0646\u0647 \u0646\u062C\u0645\u0627\u064B \u0646\u064A\u0648\u062A\u0631\u0648\u0646\u064A\u0627\u064B."@ar . . . . . . . . . "\u8D85\u65B0\u661F"@zh . . . . . . . "Supernova"@pt . . . . . "Supernova"@es . . . . . . . . . . . . . . . . . . . . . . "A supernova is a powerful and luminous explosion of a star. It has the plural form supernovae /-vi\u02D0/ or supernovas, and is abbreviated SN or SNe. This transient astronomical event occurs during the last evolutionary stages of a massive star or when a white dwarf is triggered into runaway nuclear fusion. The original object, called the progenitor, either collapses to a neutron star or black hole, or is completely destroyed. The peak optical luminosity of a supernova can be comparable to that of an entire galaxy before fading over several weeks or months."@en . . . . . . . . . . . . . . . . . . . . . . . "Una supernova (plurale supernove, in latino supernovae; abbreviata come SN o SNe) \u00E8 un'esplosione stellare pi\u00F9 energetica di quella di una nova. Le supernove sono molto luminose e causano una emissione di radiazione che pu\u00F2 per brevi periodi superare quella di una intera galassia. Durante un intervallo di tempo che pu\u00F2 andare da qualche settimana a qualche mese, una supernova emette tanta energia quanta \u00E8 previsto che ne emetta il Sole durante la sua intera esistenza e, per una quindicina di secondi, raggiunge una temperatura di cento miliardi di Kelvin, ma perch\u00E9 ci\u00F2 avvenga, la stella deve avere una massa almeno nove volte superiore a quella del nostro Sole. L'esplosione espelle la maggior parte o tutto il materiale che costituisce la stella a velocit\u00E0 che possono arrivare a 30 000 km/s (10% della velocit\u00E0 della luce), producendo un'onda d'urto che si diffonde nel mezzo interstellare. Ci\u00F2 si traduce in una bolla di gas in espansione che viene chiamata resto di supernova. Il termine nova, che significa \"nuova\" in latino, si riferisce a ci\u00F2 che appare essere una nuova stella brillante nella volta celeste. Il prefisso \"super-\" distingue le supernove dalle nove ordinarie che sono molto meno luminose. La parola supernova fu utilizzata per la prima volta da Walter Baade e Fritz Zwicky nel 1931. Le supernove possono essere innescate in due modi: o tramite la riaccensione improvvisa dei processi di fusione nucleare in una stella degenere o tramite il collasso del nucleo di una stella massiccia. Nonostante nessuna supernova sia stata osservata nella Via Lattea da SN 1604, i resti di supernova esistenti indicano che eventi di questo tipo occorrono mediamente circa tre volte ogni secolo nella nostra galassia. Essi giocano un ruolo significativo nell'arricchimento del mezzo interstellare di elementi chimici pesanti. Inoltre, la bolla di gas in espansione creata dall'esplosione pu\u00F2 portare alla formazione di nuove stelle."@it . . "En supernova \u00E4r en exploderande eller en exploderad stj\u00E4rna. Supernovorna h\u00F6r till de v\u00E5ldsammaste h\u00E4ndelserna i universum. I en supernova utvecklas oerh\u00F6rda m\u00E4ngder energi som l\u00E4mnar reststj\u00E4rnan i form av enorma neutrinofl\u00F6den, gasmassor och str\u00E5lning, vilket g\u00F6r att de under en viss tid kan lysa upp till hundra miljarder g\u00E5nger starkare \u00E4n v\u00E5r sol. Det \u00E4r lika mycket som lyskraften i en hel galax. En supernova intr\u00E4ffar dock inte s\u00E4rskilt ofta, man brukar s\u00E4ga att i en typisk galax intr\u00E4ffar detta ungef\u00E4r en g\u00E5ng vart femtionde \u00E5r. De flesta supernovorna \u00E4r dock dolda av stoft och gas och kan inte observeras. I Vintergatan r\u00E4knar man med ungef\u00E4r tre, fr\u00E5n jorden synliga supernovor per tusen \u00E5r."@sv . . . . . . . "Eine Supernova (von lateinisch stella nova, super \u201Aneuer Stern, dar\u00FCber hinaus\u2018; Plural Supernovae) ist das kurzzeitige, helle Aufleuchten eines massereichen Sterns am Ende seiner Lebenszeit durch eine Explosion, bei welcher der urspr\u00FCngliche Stern selbst vernichtet wird. Die Leuchtkraft des Sterns nimmt dabei millionen- bis milliardenfach zu, er wird f\u00FCr kurze Zeit so hell wie eine ganze Galaxie. Man kennt zwei grunds\u00E4tzliche Mechanismen, nach denen Sterne zur Supernova werden k\u00F6nnen:"@de . . . . . . "A supernova is a powerful and luminous explosion of a star. It has the plural form supernovae /-vi\u02D0/ or supernovas, and is abbreviated SN or SNe. This transient astronomical event occurs during the last evolutionary stages of a massive star or when a white dwarf is triggered into runaway nuclear fusion. The original object, called the progenitor, either collapses to a neutron star or black hole, or is completely destroyed. The peak optical luminosity of a supernova can be comparable to that of an entire galaxy before fading over several weeks or months. Supernovae are more energetic than novae. In Latin, nova means \"new\", referring astronomically to what appears to be a temporary new bright star. Adding 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 1929. The last supernova to be directly observed in the Milky Way was Kepler's Supernova in 1604, appearing not long after the also naked-eye visible SN 1572, but the remnants of more recent supernovae have been found. Observations of supernovae in other galaxies suggest they occur in the Milky Way on average about three times every century. These supernovae would almost certainly be observable with modern astronomical telescopes. 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. Theoretical studies indicate that most supernovae are triggered by one of two basic mechanisms: the sudden re-ignition of nuclear fusion in a degenerate star such as a white dwarf, or the sudden gravitational collapse of a massive star's core. In the first class of events, the object's temperature is raised enough to trigger runaway nuclear fusion, completely disrupting the star. Possible causes are an accumulation of material from a binary companion through accretion, or a stellar merger. In the massive star case, the core of a massive star may undergo sudden collapse once it is unable to produce sufficient energy from fusion to counteract the star's own gravity. While some observed supernovae are more complex than these two simplified theories, the astrophysical mechanics are established and accepted by the astronomical community. Supernovae can expel several solar masses of material at velocities up to several percent of the speed of light. 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 are a major source of elements in the interstellar medium from oxygen to rubidium. The expanding shock waves of supernovae can trigger the formation of new stars. Supernova are a major source of cosmic rays. Supernovae might produce gravitational waves, though thus far, gravitational waves have been detected only from the mergers of black holes and neutron stars."@en . . . . . "178967"^^ . . . . . "Supernova"@cs . . . . "Uma supernova \u00E9 uma explos\u00E3o estelar poderosa e luminosa. Este evento astron\u00F4mico transit\u00F3rio ocorre durante os \u00FAltimos est\u00E1gios evolutivos de uma estrela massiva ou quando uma an\u00E3 branca inicia uma fus\u00E3o nuclear descontrolada. O objeto original, chamado de progenitor, pode colapsar em uma estrela de n\u00EAutrons ou em um buraco negro, podendo ainda ser completamente destru\u00EDdo. O pico de luminosidade \u00F3ptica de uma supernova pode ser compar\u00E1vel ao de uma gal\u00E1xia inteira e demora v\u00E1rias semanas ou meses at\u00E9 desaparecer."@pt . "The Crab Nebula is a pulsar wind nebula associated with the 1054 supernova."@en . "En supernova \u00E4r en exploderande eller en exploderad stj\u00E4rna. Supernovorna h\u00F6r till de v\u00E5ldsammaste h\u00E4ndelserna i universum. I en supernova utvecklas oerh\u00F6rda m\u00E4ngder energi som l\u00E4mnar reststj\u00E4rnan i form av enorma neutrinofl\u00F6den, gasmassor och str\u00E5lning, vilket g\u00F6r att de under en viss tid kan lysa upp till hundra miljarder g\u00E5nger starkare \u00E4n v\u00E5r sol. Det \u00E4r lika mycket som lyskraften i en hel galax. En supernova intr\u00E4ffar dock inte s\u00E4rskilt ofta, man brukar s\u00E4ga att i en typisk galax intr\u00E4ffar detta ungef\u00E4r en g\u00E5ng vart femtionde \u00E5r. De flesta supernovorna \u00E4r dock dolda av stoft och gas och kan inte observeras. I Vintergatan r\u00E4knar man med ungef\u00E4r tre, fr\u00E5n jorden synliga supernovor per tusen \u00E5r. Om en supernova skulle f\u00F6rekomma inom 100\u2013200 ljus\u00E5rs avst\u00E5nd fr\u00E5n jorden kunde det inneb\u00E4ra jordens underg\u00E5ng. Nu finns det dock inga tecken p\u00E5 att n\u00E5gon av stj\u00E4rnorna inom det omr\u00E5det \u00E4r p\u00E5 v\u00E4g att bli en supernova p\u00E5 l\u00E4nge. Den senaste supernovan man har kunnat se med blotta \u00F6gat observerades \u00E5r 1987 i det Stora magellanska molnet och var mycket viktig f\u00F6r forskningen kring supernovor. Supernovan namngavs SN 1987A. Stj\u00E4rnan som exploderade var av typ II (ljus j\u00E4ttestj\u00E4rna) och dog endast 10 miljoner \u00E5r gammal, vilket \u00E4r t\u00E4mligen normalt f\u00F6r stj\u00E4rnor av den storleken. Som j\u00E4mf\u00F6relse kan n\u00E4mnas att solen ber\u00E4knas bli 12 miljarder \u00E5r gammal."@sv . . . "Supernova (jamak Supernovae) adalah ledakan yang sangat energik dari suatu bintang besar dan masif yang berada di titik tertentu dalam siklus hidupnya, yang disebabkan oleh keruntuhan inti gravitasi di mana dapat memancarkan energi lebih banyak daripada nova dan kecerahannya dapat bertahan hingga beberapa bulan. Ini biasanya terjadi ketika fusi nuklirnya tidak dapat menahan inti dari gravitasinya sendiri dan akhirnya inti runtuh dan meledak. Peristiwa supernova ini menandai berakhirnya riwayat suatu bintang. Supernova adalah objek sementara. Bintang yang mengalami supernova akan tampak sangat cemerlang dan bahkan kecemerlangannya bisa mencapai satu miliar kali cahaya semula bintang tersebut (yang dapat mengungguli seluruh galaksi), setelah beberapa minggu akhirnya meredup, dan lenyap. Kare"@in . "Una supernova (plurale supernove, in latino supernovae; abbreviata come SN o SNe) \u00E8 un'esplosione stellare pi\u00F9 energetica di quella di una nova. Le supernove sono molto luminose e causano una emissione di radiazione che pu\u00F2 per brevi periodi superare quella di una intera galassia."@it . . "( \uC74C\uC545 \uADF8\uB8F9\uC5D0 \uB300\uD574\uC11C\uB294 \uCD08\uC2E0\uC131 (\uC74C\uC545 \uADF8\uB8F9) \uBB38\uC11C\uB97C \uCC38\uACE0\uD558\uC2ED\uC2DC\uC624.) \uCD08\uC2E0\uC131(supernova)(\u8D85\u65B0\u661F)\uC740 \uC2E0\uC131(nova)\uBCF4\uB2E4 \uC5D0\uB108\uC9C0\uAC00 \uD070 \uBCC4\uC758 \uD3ED\uBC1C\uC744 \uC758\uBBF8\uD55C\uB2E4. \uCD08\uC2E0\uC131\uC740 \uADF8 \uAD11\uB3C4\uAC00 \uADF9\uB3C4\uB85C \uB192\uC73C\uBA70, \uD3ED\uBC1C\uC801\uC778 \uBC29\uC0AC\uC120\uC744 \uC77C\uC73C\uD0A4\uAE30\uC5D0, \uC5B4\uB450\uC6CC\uC9C8 \uB54C\uAE4C\uC9C0 \uC218 \uC8FC \uB610\uB294 \uC218 \uAC1C\uC6D4\uC5D0 \uAC78\uCCD0 \uD55C\uAC1C \uC740\uD558 \uC804\uCCB4\uC5D0 \uD544\uC801\uD558\uB294 \uBC1D\uAE30\uB85C \uBE5B\uB09C\uB2E4. \uC774 \uC9E7\uC740 \uAE30\uAC04 \uB3D9\uC548 \uCD08\uC2E0\uC131\uC740 \uD0DC\uC591\uC774 \uD3C9\uC0DD\uC5D0 \uAC78\uCCD0 \uBC1C\uC0B0\uD560 \uAC83\uC73C\uB85C \uCD94\uCE21\uB418\uB294 \uC5D0\uB108\uC9C0\uB9CC\uD07C\uC758 \uBC29\uC0AC\uC120 \uBCF5\uC0AC\uB97C \uBC1C\uD55C\uB2E4. \uD3ED\uBC1C\uC758 \uACB0\uACFC \uD56D\uC131\uC740 \uAD6C\uC131 \uBB3C\uC9C8\uC758 \uB300\uBD80\uBD84 \uB610\uB294 \uC804\uCCB4\uB97C \uD1A0\uD574\uB0B8\uB2E4. \uC774\uB54C \uADF8 \uC18D\uB3C4\uB294 30,000 km/s(\uAD11\uC18D\uC758 10%)\uAE4C\uC9C0 \uAC00\uC18D\uB418\uBA70, \uC8FC\uC704 \uC131\uAC04 \uB9E4\uC9C8\uC5D0 \uCDA9\uACA9\uD30C\uB97C \uC77C\uC73C\uD0A8\uB2E4. \uCDA9\uACA9\uD30C\uAC00 \uD729\uC4F8\uACE0 \uAC04 \uC790\uB9AC\uC5D0\uB294 \uD33D\uCC3D\uD558\uB294 \uAC00\uC2A4\uC640 \uBA3C\uC9C0\uC758 \uAECD\uC9C8\uC774 \uB0A8\uAC8C \uB418\uACE0, \uC774\uAC83\uC744 \uCD08\uC2E0\uC131 \uC794\uD574\uB77C\uACE0 \uBD80\uB978\uB2E4. \u2018\uC2E0\uC131\u2019(Nova)\uC774\uB780 \u2018\uC0C8\uB85C\uC6B4\u2019\uC774\uB77C\uB294 \uC758\uBBF8\uC758 \uB77C\uD2F4\uC5B4 \uB0B1\uB9D0\uC5D0\uC11C \uC720\uB798\uB41C \uAC83\uC73C\uB85C, \uCC9C\uAD6C\uC0C1\uC5D0 \uB9E4\uC6B0 \uBC1D\uC740 \uBCC4\uC774 \uC0C8\uB85C \uB098\uD0C0\uB09C \uAC83\uCC98\uB7FC \uBCF4\uC774\uB294 \uAC83\uC744 \uCE6D\uD55C \uAC83\uC774\uBA70, \uC811\uB450\uC0AC \u2018\uCD08-\u2019(super-)\uB294 \uCD08\uC2E0\uC131\uC774 \uAD11\uB3C4\uAC00 \uD6E8\uC52C \uB5A8\uC5B4\uC9C0\uB294 \uBCF4\uD1B5\uC758 \uC2E0\uC131\uACFC\uB294 \uAD6C\uBD84\uB418\uB294 \uC874\uC7AC\uB77C\uB294 \uAC83\uC744 \uC758\uBBF8\uD55C\uB2E4. \u2018\uCD08\uC2E0\uC131\u2019(supernova)\uC774\uB77C\uB294 \uB2E8\uC5B4\uB294 1931\uB144\uC5D0 \uBC1C\uD130 \uBC14\uB370\uC640 \uD504\uB9AC\uCE20 \uCE20\uBE44\uD0A4\uAC00 \uB9CC\uB4E4\uC5B4\uB0B8 \uC870\uC5B4\uC774\uB2E4."@ko . . "Supernova (jamak Supernovae) adalah ledakan yang sangat energik dari suatu bintang besar dan masif yang berada di titik tertentu dalam siklus hidupnya, yang disebabkan oleh keruntuhan inti gravitasi di mana dapat memancarkan energi lebih banyak daripada nova dan kecerahannya dapat bertahan hingga beberapa bulan. Ini biasanya terjadi ketika fusi nuklirnya tidak dapat menahan inti dari gravitasinya sendiri dan akhirnya inti runtuh dan meledak. Peristiwa supernova ini menandai berakhirnya riwayat suatu bintang. Supernova adalah objek sementara. Bintang yang mengalami supernova akan tampak sangat cemerlang dan bahkan kecemerlangannya bisa mencapai satu miliar kali cahaya semula bintang tersebut (yang dapat mengungguli seluruh galaksi), setelah beberapa minggu akhirnya meredup, dan lenyap. Karena alasan ini, benda-benda tersebut sulit untuk diamati dan dipelajari, para astronom kini telah membuat pencarian supernova yang didedikasikan untuk mencari supernova baru dan memperoleh pengamatan yang cepat dan ekstensif. Beberapa minggu atau bulan sebelum suatu bintang mengalami supernova, bintang tersebut akan melepaskan energi yang setara dengan energi matahari yang dilepaskan matahari seumur hidupnya, ledakan ini meruntuhkan sebagian besar material bintang dengan kecepatan 10.000 - 30.000 km/s (beberapa hingga 10% tahun cahaya) dan melepaskan gelombang kejut yang mampu memusnahkan medium antarbintang. Ini menyapu cangkang gas dan debu yang mengambang, yang dikenal sebagai sisa supernova. Supernova dapat secara singkat mengungguli seluruh galaksi dan memancarkan lebih banyak energi daripada Matahari kita seumur hidupnya. Para astronom membagi supernova menjadi 2 jenis utama, Tipe I dan II tergantung pada kurva cahaya dan sifat spektrumnya, baik menghentikan atau mengaktifkan produksi energi melalui fusi nuklir. Supernova tipe I kemungkinan besar bisa terbentuk sebagai katai putih yang mencuri gas panas dari bintang pendampingnya. Jika cukup banyak gas yang menumpuk di permukaan katai putih, ledakan termonuklir yang tak terkendali akan menghancurkan bintang itu berkeping-keping tanpa meninggalkan apapun. Ini adalah supernova paling terang, dan dapat mengukur jarak ke galaksi lain. Supernova tipe II adalah tahap terakhir dalam evolusi bintang masif tua yang setidaknya 8 kali lebih masif dari Matahari yang runtuh. Bintang seperti itu mencapai titik di mana ia tidak dapat lagi menghasilkan energi nuklir di intinya. Tanpa tekanan luar yang diciptakan energi ini, gravitasi menang dan menyebabkan inti bintang runtuh. Perbedaan di antara keduanya adalah supernova tipe I tidak memiliki dalam spektrumnya, sementara supernova tipe II memiliki garis hidrogennya. Setelah inti bintang yang sudah tua berhenti menghasilkan energi, maka bintang tersebut akan mengalami keruntuhan gravitasi secara tiba-tiba dan meninggalkan sisa supernova, bintang berukuran sedang (antara dua hingga massa matahari) akan menjadi bintang neutron yang sangat padat, dan jika massa yang tersisa cukup besar (lebih dari lima kali massa matahari) sehingga gravitasi meruntuhkan inti hingga menjadi lubang hitam, dan melepaskan energi potensial gravitasi yang memanaskan dan menghancurkan lapisan terluar bintang. Bintang yang lebih kecil (yang ukurannya serupa dengan Matahari) akan menjadi katai putih. Rata-rata supernova terjadi setiap 50 tahun sekali di galaksi seukuran galaksi Bima Sakti. Supernova memiliki peran dalam memperkaya medium antarbintang dengan elemen-elemen massa yang lebih besar. Kemudian, gelombang kejut dari ledakan supernova dapat membentuk formasi bintang baru."@in . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . "Een supernova (meervoud: supernovae of supernova's) is het verschijnsel waarbij een ster op spectaculaire wijze explodeert. De uitbarsting is herkenbaar aan de enorme hoeveelheid licht die hierbij wordt uitgestraald. De ster vlamt op met de lichtkracht van honderden miljoenen tot meer dan een miljard zonnen. De sterkste supernovae worden hypernova genoemd. Supernovae ontstaan via twee mechanismen: ten eerste zijn ze het natuurlijke levenseinde van alle zware sterren (supernovae van de typen Ib, Ic en II); ten tweede kunnen witte dwergen in nauwe dubbelsterren zich ontwikkelen tot een supernova (type Ia). De chemische elementen met een atoomnummer groter dan dat van ijzer danken hun ontstaan aan supernovae door middel van neutronenvangst."@nl . . . . "\u041D\u0430\u0434\u043D\u043E\u0432\u0430\u0301 (\u0430\u043D\u0433\u043B. SuperNova) \u2014 \u0437\u043E\u0440\u044F, \u0449\u043E \u0440\u0430\u043F\u0442\u043E\u0432\u043E \u0437\u0431\u0456\u043B\u044C\u0448\u0443\u0454 \u0441\u0432\u043E\u044E \u0441\u0432\u0456\u0442\u043D\u0456\u0441\u0442\u044C \u0443 \u043C\u0456\u043B\u044C\u044F\u0440\u0434\u0438 \u0440\u0430\u0437\u0456\u0432 (\u043D\u0430 20 \u0437\u043E\u0440\u044F\u043D\u0438\u0445 \u0432\u0435\u043B\u0438\u0447\u0438\u043D), \u0430 \u0456\u043D\u043E\u0434\u0456 \u0439 \u0431\u0456\u043B\u044C\u0448\u0435."@uk . . . . . . . . . . . . . . . . . . . . . . "27680"^^ . . . . . "200"^^ . . "\u0627\u0644\u0645\u064F\u0633\u0652\u062A\u064E\u0639\u0650\u0631\u064F \u0627\u0644\u0623\u0639\u0638\u0645 (Supernova \u0633\u0648\u0628\u0631\u0646\u0648\u0641\u0627) \u0647\u0648 \u062D\u062F\u062B \u0641\u0644\u0643\u064A \u064A\u062D\u062F\u062B \u062E\u0644\u0627\u0644 \u0627\u0644\u0645\u0631\u0627\u062D\u0644 \u0627\u0644\u062A\u0637\u0648\u0631\u064A\u0629 \u0627\u0644\u0623\u062E\u064A\u0631\u0629 \u0644\u062D\u064A\u0627\u0629 \u0646\u062C\u0645 \u0636\u062E\u0645\u060C \u062D\u064A\u062B \u064A\u062D\u062F\u062B \u0627\u0646\u0641\u062C\u0627\u0631 \u0646\u062C\u0645\u064A \u0647\u0627\u0626\u0644 \u064A\u0642\u0630\u0641 \u0641\u064A\u0647\u0650 \u0627\u0644\u0646\u062C\u0645 \u0628\u063A\u0644\u0627\u0641\u0647\u0650 \u0641\u064A \u0627\u0644\u0641\u0636\u0627\u0621 \u0639\u0646\u062F \u0646\u0647\u0627\u064A\u0629 \u0639\u0645\u0631\u0647\u060C \u0648\u064A\u0624\u062F\u064A \u0630\u0644\u0643 \u0625\u0644\u0649 \u062A\u0643\u0648\u0646 \u0633\u062D\u0627\u0628\u0629 \u0643\u0631\u0648\u064A\u0629 \u062D\u0648\u0644 \u0627\u0644\u0646\u062C\u0645\u060C \u0648\u0628\u0631\u0627\u0642\u0629 \u0644\u0644\u063A\u0627\u064A\u0629 (\u0634\u062F\u064A\u062F\u0629 \u0627\u0644\u0628\u0631\u064A\u0642) \u0645\u0646 \u0627\u0644\u0628\u0644\u0627\u0632\u0645\u0627\u060C \u0648\u0633\u0631\u0639\u0627\u0646 \u0645\u0627 \u062A\u0646\u062A\u0634\u0631 \u0637\u0627\u0642\u0629 \u0627\u0644\u0627\u0646\u0641\u062C\u0627\u0631 \u0641\u064A \u0627\u0644\u0641\u0636\u0627\u0621 \u0648\u062A\u062A\u062D\u0648\u0644 \u0625\u0644\u0649 \u0623\u062C\u0633\u0627\u0645 \u063A\u064A\u0631 \u0645\u0631\u0626\u064A\u0629 \u0641\u064A \u063A\u0636\u0648\u0646 \u0623\u0633\u0627\u0628\u064A\u0639 \u0623\u0648 \u0623\u0634\u0647\u0631\u060C \u0623\u0645\u0627 \u0645\u0631\u0643\u0632 \u0627\u0644\u0646\u062C\u0645 \u0641\u064A\u0646\u0647\u0627\u0631 \u0639\u0644\u0649 \u0646\u0641\u0633\u0647 \u0646\u062D\u0648 \u0627\u0644\u0645\u0631\u0643\u0632 \u0645\u0643\u0648\u0646\u0627\u064B \u0625\u0645\u0627 \u0642\u0632\u0645\u0627 \u0623\u0628\u064A\u0636\u0627 \u0623\u0648 \u064A\u062A\u062D\u0648\u0644 \u0625\u0644\u0649 \u0646\u062C\u0645 \u0646\u064A\u0648\u062A\u0631\u0648\u0646\u064A \u0648\u064A\u0639\u062A\u0645\u062F \u0630\u0644\u0643 \u0639\u0644\u0649 \u0643\u062A\u0644\u0629 \u0627\u0644\u0646\u062C\u0645\u060C \u0648\u0623\u0645\u0627 \u0625\u0630\u0627 \u0632\u0627\u062F\u062A \u0643\u062A\u0644\u0629 \u0627\u0644\u0646\u062C\u0645 \u0639\u0646 \u0646\u062D\u0648 20 \u0643\u062A\u0644\u0629 \u0634\u0645\u0633\u064A\u0629 \u0641\u0625\u0646\u0647 \u0642\u062F \u064A\u062A\u062D\u0648\u0644 \u0625\u0644\u0649 \u062B\u0642\u0628 \u0623\u0633\u0648\u062F \u0628\u062F\u0648\u0646 \u0623\u0646 \u064A\u0646\u0641\u062C\u0631 \u0641\u064A \u0635\u0648\u0631\u0629 \u0645\u0633\u062A\u0639\u0631 \u0623\u0639\u0638\u0645."@ar . "A 1414 text cites a 1055 report: since \"the baleful star appeared, a full year has passed and until now its brilliance has not faded.\""@en . . . . . . . . . "\u041D\u0430\u0434\u043D\u043E\u0432\u0430\u0301 (\u0430\u043D\u0433\u043B. SuperNova) \u2014 \u0437\u043E\u0440\u044F, \u0449\u043E \u0440\u0430\u043F\u0442\u043E\u0432\u043E \u0437\u0431\u0456\u043B\u044C\u0448\u0443\u0454 \u0441\u0432\u043E\u044E \u0441\u0432\u0456\u0442\u043D\u0456\u0441\u0442\u044C \u0443 \u043C\u0456\u043B\u044C\u044F\u0440\u0434\u0438 \u0440\u0430\u0437\u0456\u0432 (\u043D\u0430 20 \u0437\u043E\u0440\u044F\u043D\u0438\u0445 \u0432\u0435\u043B\u0438\u0447\u0438\u043D), \u0430 \u0456\u043D\u043E\u0434\u0456 \u0439 \u0431\u0456\u043B\u044C\u0448\u0435."@uk . . . . . . . . . . . "Chinese report of guest star identified as the supernova of 1054 in the Lidai mingchen zouyi .jpg"@en . . . . . . . . . . . . . "Eine Supernova (von lateinisch stella nova, super \u201Aneuer Stern, dar\u00FCber hinaus\u2018; Plural Supernovae) ist das kurzzeitige, helle Aufleuchten eines massereichen Sterns am Ende seiner Lebenszeit durch eine Explosion, bei welcher der urspr\u00FCngliche Stern selbst vernichtet wird. Die Leuchtkraft des Sterns nimmt dabei millionen- bis milliardenfach zu, er wird f\u00FCr kurze Zeit so hell wie eine ganze Galaxie. Dabei wird innerhalb von Sekunden etwa ein Foe beobachtbare Energie freigesetzt. Dies entspricht einem Wert von \u2248 3 \u00B7 1028 TWh (Terawattstunden). Zum Vergleich: h\u00E4tte die Sonne w\u00E4hrend ihrer gesamten Lebensdauer ihre derzeitige Leuchtkraft, w\u00FCrde sie 3,827 \u00B7 1026 W \u00D7 3,1536 \u00B7 107 s/Jahr \u00D7 1010 Jahre \u2248 1,2 foe an Energie freisetzen. Man kennt zwei grunds\u00E4tzliche Mechanismen, nach denen Sterne zur Supernova werden k\u00F6nnen: 1. \n* Massereiche Sterne mit einer Anfangsmasse (siehe Sternentstehung) von mehr als etwa acht Sonnenmassen, deren Kern am Ende ihrer Entwicklung und nach Verbrauch ihres nuklearen Brennstoffs kollabiert. Hierbei kann ein kompaktes Objekt, etwa ein Neutronenstern (Pulsar) oder ein Schwarzes Loch, entstehen. Dieser Vorgang wird als bzw. hydrodynamische Supernova bezeichnet. 2. \n* Sterne mit geringerer Masse, die in ihrem vorl\u00E4ufigen Endstadium als Wei\u00DFer Zwerg Material (z. B. von einem Begleiter in einem Doppelsternsystem) akkretieren, durch Eigengravitation kollabieren und dabei durch einsetzendes Kohlenstoffbrennen zerrissen werden. Dieses Ph\u00E4nomen wird als thermonukleare Supernova oder Supernova vom Typ Ia bezeichnet. Bekannte Supernovae sind die Supernova 1987A in der Gro\u00DFen Magellanschen Wolke und Keplers Supernova (1604). Speziell letztere und Tycho Brahes Supernova (1572) haben die Astronomie befl\u00FCgelt, da dadurch die klassische Auffassung von der Unver\u00E4nderlichkeit der Fixsternsph\u00E4re endg\u00FCltig widerlegt wurde. Der bekannteste Supernova\u00FCberrest ist der Krebsnebel (Supernova 1054) im Sternbild Stier."@de . . "Supernowa \u2013 termin okre\u015Blaj\u0105cy kilka rodzaj\u00F3w kosmicznych eksplozji powoduj\u0105cych powstanie na niebie niezwykle jasnego obiektu, kt\u00F3ry ju\u017C po kilku tygodniach lub miesi\u0105cach staje si\u0119 niemal niewidoczny. S\u0105 dwie mo\u017Cliwe drogi prowadz\u0105ce do takiego wybuchu: w j\u0105drze masywnej gwiazdy przesta\u0142y zachodzi\u0107 reakcje termoj\u0105drowe b\u0105d\u017A zachodzi proces poch\u0142aniaj\u0105cy promieniowanie (kreacja par, fotodezintegracja), a zmniejszenie ci\u015Bnienia promieniowania powoduje zapadanie si\u0119 gwiazdy pod w\u0142asnym ci\u0119\u017Carem, b\u0105d\u017A te\u017C bia\u0142y karze\u0142 tak d\u0142ugo pobiera\u0142 materi\u0119 z s\u0105siedniej gwiazdy, a\u017C przekroczy\u0142 mas\u0119 Chandrasekhara, co doprowadzi\u0142o do eksplozji termoj\u0105drowej. W obydwu przypadkach eksplozja supernowej z ogromn\u0105 si\u0142\u0105 wyrzuca w przestrze\u0144 wi\u0119kszo\u015B\u0107 lub ca\u0142\u0105 materi\u0119 gwiazdy. Utworzona w ten spos\u00F3b mg\u0142awica jest bardzo nietrwa\u0142a i ulega ca\u0142kowitemu rozproszeniu po okresie kilkudziesi\u0119ciu tysi\u0119cy lat, znikaj\u0105c bez \u015Bladu. Z tego powodu w Drodze Mlecznej znamy obecnie zaledwie 265 pozosta\u0142o\u015Bci po supernowych, cho\u0107 szacunkowa liczba tego rodzaju wybuch\u00F3w w ci\u0105gu ostatnich kilku miliard\u00F3w lat jest rz\u0119du wielu milion\u00F3w. Wybuch wywo\u0142uje fal\u0119 uderzeniow\u0105 rozchodz\u0105c\u0105 si\u0119 w otaczaj\u0105cej przestrzeni, formuj\u0105c mg\u0142awic\u0119 \u2013 pozosta\u0142o\u015B\u0107 po supernowej. Eksplozje supernowych s\u0105, obok kilonowych, g\u0142\u00F3wnym mechanizmem rozprzestrzeniania w kosmosie pierwiastk\u00F3w ci\u0119\u017Cszych ni\u017C tlen oraz praktycznie jedynym \u017Ar\u00F3d\u0142em pierwiastk\u00F3w ci\u0119\u017Cszych od \u017Celaza (powsta\u0142ych w spos\u00F3b naturalny). Ca\u0142y wap\u0144 w naszych ko\u015Bciach czy \u017Celazo w hemoglobinie zosta\u0142y kiedy\u015B wyrzucone w przestrze\u0144 podczas wybuchu supernowej. Supernowe wyrzuci\u0142y ci\u0119\u017Ckie pierwiastki w przestrze\u0144 mi\u0119dzygwiezdn\u0105, wzbogacaj\u0105c w ten spos\u00F3b ob\u0142oki materii b\u0119d\u0105ce miejscem formowania nowych gwiazd. Te gwa\u0142towne procesy zdeterminowa\u0142y sk\u0142ad chemiczny mg\u0142awicy s\u0142onecznej, z kt\u00F3rej 4,5 miliarda lat temu powsta\u0142 Uk\u0142ad S\u0142oneczny i ostatecznie umo\u017Cliwi\u0142y powstanie na Ziemi \u017Cycia w obecnej postaci. S\u0142owo \u201Enowa\u201D (\u0142ac. nova) oznacza now\u0105 gwiazd\u0119 pojawiaj\u0105c\u0105 si\u0119 na sferze niebieskiej; z kolei przedrostek \u201Esuper\u201D odr\u00F3\u017Cnia je od u\u017Cywanego na co dzie\u0144 s\u0142owa nowa, oznaczaj\u0105cego tak\u017Ce gwiazd\u0119 zwi\u0119kszaj\u0105c\u0105 jasno\u015B\u0107, jednak w nieco mniejszym stopniu i z innej przyczyny. Jakkolwiek nieco myl\u0105ce jest okre\u015Blanie supernowej jako nowej gwiazdy, gdy\u017C w rzeczywisto\u015Bci jest to jej \u015Bmier\u0107 (lub w najlepszym razie radykalna transformacja w co\u015B zupe\u0142nie innego)."@pl . . . . . . . . . . . . . . "\u041D\u0430\u0434\u043D\u043E\u0432\u0430"@uk . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . "Supernova"@fr . . . . . . . . "1124171611"^^ . . . . "Una supernova \u00E9s una explosi\u00F3 estel\u00B7lar tremendament energ\u00E8tica i lluminosa. Es tracta d'un esdeveniment astron\u00F2mic transitori que correspon a les fases finals de la vida d'un estel massiu o l'embalament de la fusi\u00F3 nuclear en un nan blanc. L'objecte original, el progenitor, es col\u00B7lapsa per esdevenir un estel de neutrons o un forat negre o \u00E9s destru\u00EFt. Una supernova pot arribar a brillar tant com una gal\u00E0xia sencera abans d'anar-se apagant en un per\u00EDode de setmanes o mesos. Les supernoves originen emissions de radiaci\u00F3 electromagn\u00E8tica intens\u00EDssimes que poden durar des de diverses setmanes a diversos mesos. Es caracteritzen per un r\u00E0pid augment d'intensitat fins a assolir un pic, i despr\u00E9s decreixen en brillantor de manera m\u00E9s o menys suau fins a desapar\u00E8ixer completament. Fonamentalment, s'originen a partir d'estrelles massives que ja no poden fusionar m\u00E9s el seu nucli, esgotat i incapa\u00E7 de sostenir-se per mitj\u00E0 de la dels electrons, la qual cosa les porta a contraure's sobtadament i a generar, en el proc\u00E9s, una gran emissi\u00F3 d'energia. Tamb\u00E9 existeix un altre proc\u00E9s m\u00E9s violent capa\u00E7 de generar emissions molt m\u00E9s intenses; es produeix quan una nana blanca companya d'una altra estrella, encara activa, agrega prou massa procedent de la segona com per a superar el l\u00EDmit de Chandrasekhar i procedir a la fusi\u00F3 instant\u00E0nia de tot el seu nucli, fet que genera una enorme explosi\u00F3 termonuclear que expulsa gaireb\u00E9 tot el material que la formava. Les supernoves poden alliberar de l'ordre de 10\u00D71044 joules d'energia. Per aix\u00F2, hom ha adoptat el foe (equivalent a 10\u00D71044 J) com a unitat est\u00E0ndard per mesurar l'energia de les supernoves. Les supernoves provoquen l'expulsi\u00F3 de les capes superficials de l'estrella en forma d'enormes ones de xoc, omplint l'espai que les envolta amb elements pesants, que originen n\u00FAvols de pols i gas. Quan el front d'ona de l'explosi\u00F3 arriba a altres n\u00FAvols de gas i pols propers, els comprimeix i aquest fet pot desencadenar la formaci\u00F3 de noves nebuloses que formin, posteriorment, nous sistemes estel\u00B7lars, potser amb planetes rocosos, a causa de l'esmentada pres\u00E8ncia d'elements pesants procedents de l'explosi\u00F3 de la supernova."@ca . . . . . . . . "Is \u00E9 an t-olln\u00F3va an phl\u00E9asc mhillteanach is dual do na r\u00E9alta\u00ED m\u00F3ra a dh\u00E9anamh, agus iad i ndeireadh a gcuid hidrigine. Nuair a rithfidh an hidrigin gann ar an r\u00E9alta, tos\u00F3idh na d\u00FAile n\u00EDos troime taobh istigh den r\u00E9alta \u00E1 g go d\u00FAile n\u00EDos troime f\u00F3s. Nuair a shroichfidh an fhorbairt seo n\u00FAicl\u00E9as (cro\u00EDl\u00E1r) na r\u00E9alta, cuirfear a strucht\u00FAr inmhe\u00E1nach tr\u00ED ch\u00E9ile chomh hioml\u00E1n is go s\u00E9idfear an r\u00E9alta go l\u00E9ir amach ina . Mura bhfuil an r\u00E9alta r\u00F3throm, n\u00ED fh\u00E1gfar a dhath di ach an sceall seo agus \u00E9 \u00E1 scaipeadh i ngach treo amach ins an sp\u00E1s. Ag r\u00E9alta\u00ED troma, \u00E1fach, is iad na cisil is faide amach \u00F3n gcro\u00EDl\u00E1r amh\u00E1in a phl\u00E9ascfaidh, agus an cro\u00EDl\u00E1r f\u00E9in ag imphl\u00E9ascadh - is \u00E9 sin, ag crapadh isteach chuige f\u00E9in faoi bhr\u00FA na pl\u00E9isce agus a imtharraingthe f\u00E9in le hiomp\u00FA ina neodr\u00F3nr\u00E9alta n\u00F3 ina dh\u00FApholl. N\u00ED m\u00F3r cuimhne a choinne\u00E1il air nach ionann n\u00F3va agus olln\u00F3va, n\u00F3 is \u00F3c\u00E1id aonair \u00E9 an t-olln\u00F3va nach bhf\u00E1gann a seanbhail ar an r\u00E9alta a thuilleadh. Cuid mh\u00F3r de na n\u00F3va\u00ED, is iad a thiteann amach ar\u00EDs, fi\u00FA go tr\u00E1thrialta."@ga . . . . . . . . . . . "Supernoba"@eu . . . 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"Supernova"@de . . . . "Supernoba noba bat baino indar handiagoz lehertzen den izarra da, eta leherketari berari ere supernoba deritzo. Supernobek hainbat astez edota hilabetez irauten duten oso argi-izpi distiratsuak igortzen dituzte. Fenomeno hori oso masa handiko izarretan sortzen da, gehiago fusionatu ezin dutenean. Hori gertatzen denean, bat-batean uzkurtzen dira, eta ondoren energia handia igortzen dute. Izarrak eztanda egiten duenean, ehun mila edo milioi bat aldiz handitzen da haren argitasuna; hala, izar hil berria egun batzuetan galaxia bat bezain argitsu izaten da, eta kanpoko geruzak segundoko milaka kilometroko abiaduraz jaurtitzen ditu espaziora. Supernoba noba baten antzekoa da: biek ala biek egun gutxi batzuk baino ez dute irauten; hasieran, argitasun bizia eta handia izaten dute, eta gerora jarraian galtzen dute argia. Supernoba-leherketa bat, ordea, izarrarentzat kataklismo-gertaera da, izarraren bizitza aktiboaren amaiera, alegia."@eu . . . . . . 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"Una supernova (del lat\u00EDn nova, \u00ABnueva\u00BB) es una explosi\u00F3n estelar que puede manifestarse de forma muy notable en el espacio, incluso a simple vista, en lugares de la esfera celeste donde antes no se hab\u00EDa detectado nada en particular. Por esta raz\u00F3n, a eventos de esta naturaleza se los llam\u00F3 inicialmente stellae novae (\u00ABestrellas nuevas\u00BB) o simplemente novae. Con el tiempo se hizo la distinci\u00F3n entre fen\u00F3menos aparentemente similares pero de luminosidad intr\u00EDnseca muy diferente; los menos luminosos continuaron llam\u00E1ndose novae (novas), en tanto que el t\u00E9rmino supernova fue acu\u00F1ado por Walter Baade y Fritz Zwicky en 1931 para denominar a los m\u00E1s luminosos agreg\u00E1ndoles el prefijo \u00ABsuper-\u00BB."@es . . "Supernova"@in . . "Supernovao"@eo . . . . . . . . . . . . . . . . . . . . "Supernova"@en . . . . . . . "Crab Nebula.jpg"@en . . . "( \uC74C\uC545 \uADF8\uB8F9\uC5D0 \uB300\uD574\uC11C\uB294 \uCD08\uC2E0\uC131 (\uC74C\uC545 \uADF8\uB8F9) \uBB38\uC11C\uB97C \uCC38\uACE0\uD558\uC2ED\uC2DC\uC624.) \uCD08\uC2E0\uC131(supernova)(\u8D85\u65B0\u661F)\uC740 \uC2E0\uC131(nova)\uBCF4\uB2E4 \uC5D0\uB108\uC9C0\uAC00 \uD070 \uBCC4\uC758 \uD3ED\uBC1C\uC744 \uC758\uBBF8\uD55C\uB2E4. \uCD08\uC2E0\uC131\uC740 \uADF8 \uAD11\uB3C4\uAC00 \uADF9\uB3C4\uB85C \uB192\uC73C\uBA70, \uD3ED\uBC1C\uC801\uC778 \uBC29\uC0AC\uC120\uC744 \uC77C\uC73C\uD0A4\uAE30\uC5D0, \uC5B4\uB450\uC6CC\uC9C8 \uB54C\uAE4C\uC9C0 \uC218 \uC8FC \uB610\uB294 \uC218 \uAC1C\uC6D4\uC5D0 \uAC78\uCCD0 \uD55C\uAC1C \uC740\uD558 \uC804\uCCB4\uC5D0 \uD544\uC801\uD558\uB294 \uBC1D\uAE30\uB85C \uBE5B\uB09C\uB2E4. \uC774 \uC9E7\uC740 \uAE30\uAC04 \uB3D9\uC548 \uCD08\uC2E0\uC131\uC740 \uD0DC\uC591\uC774 \uD3C9\uC0DD\uC5D0 \uAC78\uCCD0 \uBC1C\uC0B0\uD560 \uAC83\uC73C\uB85C \uCD94\uCE21\uB418\uB294 \uC5D0\uB108\uC9C0\uB9CC\uD07C\uC758 \uBC29\uC0AC\uC120 \uBCF5\uC0AC\uB97C \uBC1C\uD55C\uB2E4. \uD3ED\uBC1C\uC758 \uACB0\uACFC \uD56D\uC131\uC740 \uAD6C\uC131 \uBB3C\uC9C8\uC758 \uB300\uBD80\uBD84 \uB610\uB294 \uC804\uCCB4\uB97C \uD1A0\uD574\uB0B8\uB2E4. \uC774\uB54C \uADF8 \uC18D\uB3C4\uB294 30,000 km/s(\uAD11\uC18D\uC758 10%)\uAE4C\uC9C0 \uAC00\uC18D\uB418\uBA70, \uC8FC\uC704 \uC131\uAC04 \uB9E4\uC9C8\uC5D0 \uCDA9\uACA9\uD30C\uB97C \uC77C\uC73C\uD0A8\uB2E4. \uCDA9\uACA9\uD30C\uAC00 \uD729\uC4F8\uACE0 \uAC04 \uC790\uB9AC\uC5D0\uB294 \uD33D\uCC3D\uD558\uB294 \uAC00\uC2A4\uC640 \uBA3C\uC9C0\uC758 \uAECD\uC9C8\uC774 \uB0A8\uAC8C \uB418\uACE0, \uC774\uAC83\uC744 \uCD08\uC2E0\uC131 \uC794\uD574\uB77C\uACE0 \uBD80\uB978\uB2E4. \u2018\uC2E0\uC131\u2019(Nova)\uC774\uB780 \u2018\uC0C8\uB85C\uC6B4\u2019\uC774\uB77C\uB294 \uC758\uBBF8\uC758 \uB77C\uD2F4\uC5B4 \uB0B1\uB9D0\uC5D0\uC11C \uC720\uB798\uB41C \uAC83\uC73C\uB85C, \uCC9C\uAD6C\uC0C1\uC5D0 \uB9E4\uC6B0 \uBC1D\uC740 \uBCC4\uC774 \uC0C8\uB85C \uB098\uD0C0\uB09C \uAC83\uCC98\uB7FC \uBCF4\uC774\uB294 \uAC83\uC744 \uCE6D\uD55C \uAC83\uC774\uBA70, \uC811\uB450\uC0AC \u2018\uCD08-\u2019(super-)\uB294 \uCD08\uC2E0\uC131\uC774 \uAD11\uB3C4\uAC00 \uD6E8\uC52C \uB5A8\uC5B4\uC9C0\uB294 \uBCF4\uD1B5\uC758 \uC2E0\uC131\uACFC\uB294 \uAD6C\uBD84\uB418\uB294 \uC874\uC7AC\uB77C\uB294 \uAC83\uC744 \uC758\uBBF8\uD55C\uB2E4. \u2018\uCD08\uC2E0\uC131\u2019(supernova)\uC774\uB77C\uB294 \uB2E8\uC5B4\uB294 1931\uB144\uC5D0 \uBC1C\uD130 \uBC14\uB370\uC640 \uD504\uB9AC\uCE20 \uCE20\uBE44\uD0A4\uAC00 \uB9CC\uB4E4\uC5B4\uB0B8 \uC870\uC5B4\uC774\uB2E4. \uCD08\uC2E0\uC131\uC774 \uC0DD\uC131\uB420 \uC218 \uC788\uB294 \uBC29\uBC95\uC740 \uC8FD\uC740 \uBCC4\uC5D0 \uAC11\uC791\uC2A4\uB7EC\uC6B4 \uD575\uC735\uD569 \uC7AC\uC810\uD654\uAC00 \uC77C\uC5B4\uB098\uAC70\uB098, \uB610\uB294 \uAC70\uB300\uD55C \uBCC4\uC758 \uC911\uC2EC\uD575\uC774 \uBD95\uAD34\uD558\uAC70\uB098 \uB450 \uAC00\uC9C0\uAC00 \uC788\uB2E4. \uBCC4\uC758 \uC2DC\uCCB4\uB77C\uACE0 \uD560 \uC218 \uC788\uB294 \uBC31\uC0C9 \uC65C\uC131\uC774 \uB3D9\uBC18\uC131\uC73C\uB85C\uBD80\uD130 \uBB3C\uC9C8\uC744 \uBE7C\uC557\uC544 \uAC08 \uB54C, \uAC15\uCC29 \uD604\uC0C1\uC774 \uC77C\uC5B4\uB098\uAC70\uB098 \uC544\uC608 \uB3D9\uBC18\uC131\uACFC \uD558\uB098\uAC00 \uB418\uAC70\uB098 \uD558\uC5EC, \uBE7C\uC557\uC740 \uBB3C\uC9C8\uC774 \uCDA9\uBD84\uD788 \uB204\uC801\uB418\uBA74 \uBC31\uC0C9 \uC65C\uC131\uC758 \uC911\uC2EC\uD575 \uC628\uB3C4\uAC00 \uC0C1\uC2B9\uD558\uC5EC \uAC00 \uC77C\uC5B4\uB09C\uB2E4. \uADF8\uB9AC\uD558\uC5EC \uD0C4\uC18C \uD575\uC735\uD569\uC5D0 \uBD88\uC774 \uBD99\uC73C\uBA74 \uC5F4\uD3ED\uC8FC\uAC00 \uC77C\uC5B4\uB098 \uBCC4\uC744 \uC644\uC804\uD788 \uD30C\uC5F4\uC2DC\uD0A4\uAC8C \uB41C\uB2E4. \uB610\uB294 \uC9C8\uB7C9\uC774 \uAC70\uB300\uD55C \uBCC4\uC758 \uC911\uC2EC\uD575\uC774 \uAC11\uC791\uC2A4\uB7F0 \uC911\uB825 \uBD95\uAD34\uB97C \uC77C\uC73C\uD0A4\uACE0, \uADF8\uB85C \uC778\uD558\uC5EC \uC911\uB825 \uC704\uCE58 \uC5D0\uB108\uC9C0\uB97C \uBC1C\uC0B0\uD560 \uB54C \uC5ED\uC2DC \uCD08\uC2E0\uC131 \uD3ED\uBC1C\uC774 \uC77C\uC5B4\uB09C\uB2E4. \uC6B0\uB9AC \uC740\uD558\uC5D0\uC11C\uB294 \uCF00\uD50C\uB7EC \uCD08\uC2E0\uC131(SN 1604) \uC774\uD6C4 \uCD08\uC2E0\uC131\uC774 \uD55C \uAC1C\uB3C4 \uBC1C\uACAC\uB418\uC9C0\uB294 \uBABB\uD588\uC9C0\uB9CC, \uCD08\uC2E0\uC131 \uC794\uD574\uB4E4\uC744 \uC0B4\uD3B4\uBCF4\uBA74 \uC6B0\uB9AC \uC740\uD558\uC5D0\uC11C\uB3C4 \uD55C \uC138\uAE30\uB2F9 \uD3C9\uADE0 \uC57D \uC138 \uBC88\uC758 \uCD08\uC2E0\uC131 \uD3ED\uBC1C \uC0AC\uAC74\uC774 \uC77C\uC5B4\uB098\uACE0 \uC788\uC74C\uC744 \uC54C \uC218 \uC788\uB2E4. \uCD08\uC2E0\uC131\uC740 \uC131\uAC04 \uB9E4\uC9C8\uC5D0 \uC9C8\uB7C9\uC774 \uD070 \uC6D0\uC18C\uC758 \uC591\uC744 \uB298\uB9AC\uB294 \uB370 \uACB0\uC815\uC801\uC778 \uC5ED\uD560\uC744 \uD55C\uB2E4(\uD575\uD569\uC131). \uBFD0\uB9CC \uC544\uB2C8\uB77C, \uCD08\uC2E0\uC131 \uD3ED\uBC1C\uB85C \uC778\uD55C \uCDA9\uACA9\uD30C\uB294 \uC0C8\uB85C\uC6B4 \uBCC4\uC758 \uD615\uC131\uC758 \uBC29\uC544\uC1E0 \uC5ED\uD560\uC744 \uD55C\uB2E4."@ko . . . 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\u0434\u0430\u043B\u0435\u0435. \u041D\u0435\u043F\u043E\u0434\u0442\u0432\u0435\u0440\u0436\u0434\u0451\u043D\u043D\u044B\u0435 \u0441\u0432\u0435\u0440\u0445\u043D\u043E\u0432\u044B\u0435 \u043E\u0431\u043E\u0437\u043D\u0430\u0447\u0430\u044E\u0442 \u0431\u0443\u043A\u0432\u0430\u043C\u0438 PSN (\u0430\u043D\u0433\u043B. possible supernova) \u0441 \u043D\u0435\u0431\u0435\u0441\u043D\u044B\u043C\u0438 \u043A\u043E\u043E\u0440\u0434\u0438\u043D\u0430\u0442\u0430\u043C\u0438 \u0432 \u0444\u043E\u0440\u043C\u0430\u0442\u0435 Jhhmmssss+ddmmsss."@ru . . . . . "Una supernova (del lat\u00EDn nova, \u00ABnueva\u00BB) es una explosi\u00F3n estelar que puede manifestarse de forma muy notable en el espacio, incluso a simple vista, en lugares de la esfera celeste donde antes no se hab\u00EDa detectado nada en particular. Por esta raz\u00F3n, a eventos de esta naturaleza se los llam\u00F3 inicialmente stellae novae (\u00ABestrellas nuevas\u00BB) o simplemente novae. Con el tiempo se hizo la distinci\u00F3n entre fen\u00F3menos aparentemente similares pero de luminosidad intr\u00EDnseca muy diferente; los menos luminosos continuaron llam\u00E1ndose novae (novas), en tanto que el t\u00E9rmino supernova fue acu\u00F1ado por Walter Baade y Fritz Zwicky en 1931 para denominar a los m\u00E1s luminosos agreg\u00E1ndoles el prefijo \u00ABsuper-\u00BB. Este evento astron\u00F3mico ocurre durante las \u00FAltimas etapas evolutivas de una estrella masiva o cuando una enana blanca se desencadena en una fusi\u00F3n nuclear descontrolada. El objeto original, llamado progenitor, se colapsa en una estrella de neutrones o un agujero negro, o se destruye por completo. El t\u00E9rmino m\u00E1s arcaico fue utilizado desde la antig\u00FCedad para indicar la explosi\u00F3n de una estrella s\u00FAper gigante roja en sus capas externas, las cuales producen una luminosidad que puede aumentar 100 000 veces su brillo original. Esta luminosidad dura unos pocos d\u00EDas y, en ocasiones, puede ser observada a simple vista desde la Tierra. Al ver un nuevo resplandor en el cielo, los seres humanos cre\u00EDan que hab\u00EDa aparecido una nueva estrella. Al a\u00F1o siguiente de la muerte de Fritz Zwicky, en agosto de 1975, apareci\u00F3 una nova que pudo ser observada a simple vista desde la Tierra, durante algunos d\u00EDas. Esta nova surgi\u00F3 de la explosi\u00F3n de una gigante roja.\u200B Las supernovas producen destellos de luz intens\u00EDsimos que pueden durar desde varias semanas a varios meses. Se caracterizan por un r\u00E1pido aumento de la intensidad luminosa hasta alcanzar una magnitud absoluta mayor que el resto de la galaxia. Posteriormente, su brillo decrece de forma m\u00E1s o menos suave hasta desaparecer completamente. Se han propuesto varios escenarios para su origen. Pueden ser estrellas masivas que ya no pueden desarrollar reacciones termonucleares en su n\u00FAcleo, y que son incapaces de sostenerse por la presi\u00F3n de degeneraci\u00F3n de los electrones, lo que las lleva a contraerse repentinamente (colapsar) y generar, en el proceso, una fuerte emisi\u00F3n de energ\u00EDa. Otro proceso m\u00E1s violento a\u00FAn, capaz de generar destellos incluso mucho m\u00E1s intensos, puede suceder cuando una enana blanca miembro de un sistema binario cerrado, recibe suficiente masa de su compa\u00F1era como para superar el l\u00EDmite de Chandrasekhar y proceder a la fusi\u00F3n instant\u00E1nea de todo su n\u00FAcleo: esto dispara una explosi\u00F3n termonuclear que expulsa casi todo, si no todo, el material que la formaba. La explosi\u00F3n de supernova provoca la expulsi\u00F3n de las capas externas de la estrella por medio de poderosas ondas de choque, enriqueciendo el espacio que la rodea con elementos pesados. Los restos eventualmente componen nubes de polvo y gas. Cuando el frente de onda de la explosi\u00F3n alcanza otras nubes de gas y polvo cercanas, las comprime y puede desencadenar la formaci\u00F3n de nuevas nebulosas solares que originan, despu\u00E9s de cierto tiempo, nuevos sistemas estelares (quiz\u00E1 con planetas, al estar las nebulosas enriquecidas con los elementos procedentes de la explosi\u00F3n). Estos residuos estelares en expansi\u00F3n se denominan remanentes y pueden tener o no un objeto compacto en su interior. Dicho remanente terminar\u00E1 por diluirse en el medio interestelar al cabo de millones de a\u00F1os. Un ejemplo es RCW 86. Las supernovas pueden liberar varias veces 1044 J de energ\u00EDa. Esto ha resultado en la adopci\u00F3n del foe (1044 J) como unidad est\u00E1ndar de energ\u00EDa en el estudio de supernovas. El 20 de septiembre de 2016, un astr\u00F3nomo aficionado llamado V\u00EDctor Buso, se convirti\u00F3 en la primera persona en la historia en fotografiar el nacimiento de una supernova a 86 millones de a\u00F1os luz, en la galaxia espiral NGC 613, al explotar la estrella bautizada SN 2016gkg. \u200B"@es . "\uCD08\uC2E0\uC131"@ko . . "\u8D85\u65B0\u661F\uFF08\u82F1\u8A9E\uFF1ASupernova\uFF09\u662F\u67D0\u4E9B\u6052\u661F\u5728\u6F14\u5316\u63A5\u8FD1\u672B\u671F\u65F6\u7ECF\u5386\u7684\u4E00\u79CD\u5267\u70C8\u7206\u70B8\u3002\u8FD9\u79CD\u7206\u70B8\u90FD\u6781\u5176\u660E\u4EAE\uFF0C\u8FC7\u7A0B\u4E2D\u6240\u7A81\u53D1\u7684\u7535\u78C1\u8F90\u5C04\u7ECF\u5E38\u80FD\u591F\u7167\u4EAE\u5176\u6240\u5728\u7684\u6574\u4E2A\u661F\u7CFB\uFF0C\u5E76\u53EF\u80FD\u6301\u7EED\u51E0\u5468\u81F3\u51E0\u4E2A\u6708\u751A\u81F3\u5E7E\u5E74\u624D\u4F1A\u9010\u6E10\u8870\u51CF\u3002\u800C\u5728\u6B64\u671F\u95F4\uFF0C\u4E00\u9897\u8D85\u65B0\u661F\u6240\u91CA\u653E\u7684\u8F90\u5C04\u80FD\u91CF\u53EF\u4EE5\u4E0E\u592A\u9633\u5728\u5176\u4E00\u751F\u4E2D\u8F90\u5C04\u80FD\u91CF\u7684\u603B\u548C\u76F8\u7576\u3002\u6052\u661F\u901A\u8FC7\u7206\u70B8\u53EF\u4EE5\u5C06\u5176\u5927\u90E8\u5206\u751A\u81F3\u51E0\u4E4E\u6240\u6709\u7269\u8D28\u4EE5\u63A5\u8FD1\u5341\u5206\u4E4B\u4E00\u5149\u901F\u7684\u901F\u5EA6\u5411\u5916\u629B\u6563\uFF0C\u5E76\u5411\u5468\u56F4\u7684\u661F\u9645\u7269\u8D28\u8F90\u5C04\u6FC0\u6CE2\u3002\u8FD9\u79CD\u6FC0\u6CE2\u4F1A\u5BFC\u81F4\u4E00\u4E2A\u7531\u81A8\u80C0\u7684\u6C14\u4F53\u548C\u5C18\u57C3\u6784\u6210\u7684\u58F3\u72B6\u7ED3\u6784\u5F62\u6210\uFF0C\u8FD9\u88AB\u79F0\u4F5C\u8D85\u65B0\u661F\u9057\u8FF9\u3002\u8D85\u65B0\u661F\u662F\u661F\u7CFB\u5F15\u529B\u6CE2\u6F5B\u5728\u7684\u5F37\u5927\u4F86\u6E90\u3002\u521D\u7D1A\u5B87\u5B99\u5C04\u7DDA\u4E2D\u5F88\u5927\u4E00\u90E8\u5206\u662F\u4F86\u81EA\u65BC\u8D85\u65B0\u661F\u3002 \u8D85\u65B0\u661F\u6BD4\u65B0\u661F\u66F4\u6709\u6D3B\u529B\u3002\u8D85\u65B0\u661F\u7684\u82F1\u6587\u540D\u7A31\u70BAsupernova\uFF0Cnova\u5728\u62C9\u4E01\u8A9E\u4E2D\u662F\u201C\u65B0\u201D\u7684\u610F\u601D\uFF0C\u9019\u8868\u793A\u5B83\u5728\u5929\u7403\u4E0A\u770B\u4E0A\u53BB\u662F\u4E00\u9846\u65B0\u51FA\u73FE\u7684\u4EAE\u661F\uFF08\u5176\u5BE6\u539F\u672C\u5373\u5DF2\u5B58\u5728\uFF0C\u56E0\u5176\u4EAE\u5EA6\u589E\u52A0\u800C\u88AB\u8AA4\u8A8D\u70BA\u662F\u65B0\u51FA\u73FE\u7684\uFF09\uFF1B\u5B57\u9996\u7684super-\u662F\u70BA\u4E86\u5C07\u8D85\u65B0\u661F\u548C\u4E00\u822C\u7684\u65B0\u661F\u6709\u6240\u5340\u5206\uFF0C\u4E5F\u8868\u793A\u8D85\u65B0\u661F\u5177\u6709\u66F4\u9AD8\u7684\u4EAE\u5EA6\u3002\u8D85\u65B0\u661F\u9019\u500B\u540D\u8A5E\u662F\u6C83\u723E\u7279\u00B7\u5DF4\u5FB7\u548C\u5F17\u91CC\u8328\u00B7\u8332\u5A01\u57FA\u57281931\u5E74\u5275\u9020\u7684\u3002"@zh . . . . . . . "Une supernova est l'ensemble des ph\u00E9nom\u00E8nes qui r\u00E9sultent de l'implosion d'une \u00E9toile en fin de vie, notamment une gigantesque explosion qui s'accompagne d'une augmentation br\u00E8ve mais fantastiquement grande de sa luminosit\u00E9. Vue depuis la Terre, une supernova appara\u00EEt donc souvent comme une \u00E9toile nouvelle, alors qu'elle correspond en r\u00E9alit\u00E9 \u00E0 la disparition d'une \u00E9toile. Bien qu'il s'en produise une toutes les deux ou trois secondes dans l'Univers observable, les supernovas sont des \u00E9v\u00E9nements rares \u00E0 l'\u00E9chelle humaine : leur taux est estim\u00E9 \u00E0 environ une \u00E0 trois par si\u00E8cle dans la Voie lact\u00E9e. Aucune supernova n'a \u00E9t\u00E9 observ\u00E9e dans notre galaxie, la Voie lact\u00E9e, depuis l'invention du t\u00E9lescope. La plus rapproch\u00E9e observ\u00E9e depuis est SN 1987A, survenue dans une galaxie voisine, le Grand Nuage de Magellan. Elles ont jou\u00E9 et jouent encore un r\u00F4le essentiel dans l'histoire de l'Univers, car c'est lors de son explosion en supernova que l'\u00E9toile lib\u00E8re les \u00E9l\u00E9ments chimiques qu'elle a synth\u00E9tis\u00E9s au cours de son existence \u2014 et pendant l'explosion m\u00EAme \u2014 et qui sont ensuite diffus\u00E9s dans le milieu interstellaire. De plus, l'onde de choc de la supernova favorise la formation de nouvelles \u00E9toiles en provoquant ou en acc\u00E9l\u00E9rant la contraction de r\u00E9gions du milieu interstellaire. Le processus \u00E0 l'origine d'une supernova est extr\u00EAmement bref : il dure quelques millisecondes. Quant au ph\u00E9nom\u00E8ne lumineux r\u00E9manent, il peut durer plusieurs mois. Au maximum de luminosit\u00E9 de l'explosion, la magnitude absolue de l'astre peut atteindre -19, ce qui en fait un objet plus lumineux de plusieurs ordres de grandeur que les \u00E9toiles les plus brillantes : pendant cette p\u00E9riode, la supernova peut \u00AB rayonner plus d'\u00E9nergie \u00BB (et donc avoir une puissance plus grande) qu'une, voire plusieurs galaxies enti\u00E8res. C'est la raison pour laquelle une supernova se produisant dans notre propre galaxie, voire une galaxie proche, est souvent visible \u00E0 l'\u0153il nu, m\u00EAme en plein jour. Plusieurs supernovas historiques ont \u00E9t\u00E9 d\u00E9crites \u00E0 des \u00E9poques parfois tr\u00E8s anciennes ; on interpr\u00E8te aujourd'hui ces apparitions d'\u00AB \u00E9toiles nouvelles \u00BB comme \u00E9tant des supernovas. Il existe deux m\u00E9canismes, en r\u00E9alit\u00E9 assez distincts, qui produisent une supernova : le premier, la supernova thermonucl\u00E9aire, r\u00E9sulte de l'explosion thermonucl\u00E9aire d'un cadavre d'\u00E9toile appel\u00E9 naine blanche ; le second, la supernova \u00E0 effondrement de c\u0153ur, suit l'implosion d'une \u00E9toile massive qui est encore le si\u00E8ge de r\u00E9actions nucl\u00E9aires au moment de l'implosion. Cette implosion est responsable de la dislocation des couches externes de l'\u00E9toile. Un troisi\u00E8me m\u00E9canisme, encore incertain, mais s'apparentant au second, est susceptible de se produire au sein des \u00E9toiles les plus massives : la supernova par production de paires. Historiquement, les supernovas \u00E9taient class\u00E9es suivant leurs caract\u00E9ristiques spectroscopiques. Cette classification \u00E9tait peu pertinente d'un point de vue physique. Seules les supernovas dites de type Ia (prononc\u00E9 \u00AB 1 a \u00BB) sont thermonucl\u00E9aires, toutes les autres \u00E9tant \u00E0 effondrement de c\u0153ur. La mati\u00E8re expuls\u00E9e par une supernova s'\u00E9tend dans l'espace, formant un type de n\u00E9buleuse appel\u00E9 r\u00E9manent de supernova. La dur\u00E9e de vie de ce type de n\u00E9buleuse est relativement limit\u00E9e, la mati\u00E8re \u00E9tant \u00E9ject\u00E9e \u00E0 tr\u00E8s grande vitesse (plusieurs milliers de kilom\u00E8tres par seconde), le r\u00E9manent se dissipe relativement vite \u00E0 l'\u00E9chelle astronomique, en quelques centaines de milliers d'ann\u00E9es. La n\u00E9buleuse de Gum ou les dentelles du Cygne sont des exemples de r\u00E9manents de supernova dans cet \u00E9tat tr\u00E8s avanc\u00E9 de dilution dans le milieu interstellaire. La n\u00E9buleuse du Crabe est un exemple de r\u00E9manent jeune : l'\u00E9clat de l'explosion qui lui a donn\u00E9 naissance a atteint la Terre il y a moins de mille ans."@fr . . . . . . . . . . . . . . . . "Supernowa \u2013 termin okre\u015Blaj\u0105cy kilka rodzaj\u00F3w kosmicznych eksplozji powoduj\u0105cych powstanie na niebie niezwykle jasnego obiektu, kt\u00F3ry ju\u017C po kilku tygodniach lub miesi\u0105cach staje si\u0119 niemal niewidoczny. S\u0105 dwie mo\u017Cliwe drogi prowadz\u0105ce do takiego wybuchu: w j\u0105drze masywnej gwiazdy przesta\u0142y zachodzi\u0107 reakcje termoj\u0105drowe b\u0105d\u017A zachodzi proces poch\u0142aniaj\u0105cy promieniowanie (kreacja par, fotodezintegracja), a zmniejszenie ci\u015Bnienia promieniowania powoduje zapadanie si\u0119 gwiazdy pod w\u0142asnym ci\u0119\u017Carem, b\u0105d\u017A te\u017C bia\u0142y karze\u0142 tak d\u0142ugo pobiera\u0142 materi\u0119 z s\u0105siedniej gwiazdy, a\u017C przekroczy\u0142 mas\u0119 Chandrasekhara, co doprowadzi\u0142o do eksplozji termoj\u0105drowej. W obydwu przypadkach eksplozja supernowej z ogromn\u0105 si\u0142\u0105 wyrzuca w przestrze\u0144 wi\u0119kszo\u015B\u0107 lub ca\u0142\u0105 materi\u0119 gwiazdy."@pl . . "vertical"@en . "Supernoba noba bat baino indar handiagoz lehertzen den izarra da, eta leherketari berari ere supernoba deritzo. Supernobek hainbat astez edota hilabetez irauten duten oso argi-izpi distiratsuak igortzen dituzte. Fenomeno hori oso masa handiko izarretan sortzen da, gehiago fusionatu ezin dutenean. Hori gertatzen denean, bat-batean uzkurtzen dira, eta ondoren energia handia igortzen dute."@eu . . "Supernovao estas giganta steleksplodo, per kiu la tuta materialo de pezega stelo (10 foje a\u016D pli ol la suna maso), escepte de \u011Dia centra kerno, di\u015Djeti\u011Das tra la interstelan spacon. La heleco de tia eksplodo estas tiel, ke foje eblas vidi \u011Din per nuda okulo en la \u0109ielo. \n* Resta\u0135o de la Keplera supernovao, kiu eksplodis la 9-an de oktobro 1604. \n* Resta\u0135oj de supernovao 1987A en Granda Magelana Nubo (en centro). Helaj blankaj objektoj maldekstre supre kaj dekstre malsupre estas la aliaj steloj. \n* Dependo de heleco de supernovao de tempo por specoj de supernovaoj II-P kaj II-L. \n*"@eo . . . . . . . . . . . . "\u03A5\u03C0\u03B5\u03C1\u03BA\u03B1\u03B9\u03BD\u03BF\u03C6\u03B1\u03BD\u03AE\u03C2 \u03B1\u03C3\u03C4\u03AD\u03C1\u03B1\u03C2"@el . . . . . . . . . . . "Supernova"@sv . . . "Een supernova (meervoud: supernovae of supernova's) is het verschijnsel waarbij een ster op spectaculaire wijze explodeert. De uitbarsting is herkenbaar aan de enorme hoeveelheid licht die hierbij wordt uitgestraald. De ster vlamt op met de lichtkracht van honderden miljoenen tot meer dan een miljard zonnen. De sterkste supernovae worden hypernova genoemd."@nl . . . . . . . . . . . . . . "Is \u00E9 an t-olln\u00F3va an phl\u00E9asc mhillteanach is dual do na r\u00E9alta\u00ED m\u00F3ra a dh\u00E9anamh, agus iad i ndeireadh a gcuid hidrigine. Nuair a rithfidh an hidrigin gann ar an r\u00E9alta, tos\u00F3idh na d\u00FAile n\u00EDos troime taobh istigh den r\u00E9alta \u00E1 g go d\u00FAile n\u00EDos troime f\u00F3s. Nuair a shroichfidh an fhorbairt seo n\u00FAicl\u00E9as (cro\u00EDl\u00E1r) na r\u00E9alta, cuirfear a strucht\u00FAr inmhe\u00E1nach tr\u00ED ch\u00E9ile chomh hioml\u00E1n is go s\u00E9idfear an r\u00E9alta go l\u00E9ir amach ina . Mura bhfuil an r\u00E9alta r\u00F3throm, n\u00ED fh\u00E1gfar a dhath di ach an sceall seo agus \u00E9 \u00E1 scaipeadh i ngach treo amach ins an sp\u00E1s. Ag r\u00E9alta\u00ED troma, \u00E1fach, is iad na cisil is faide amach \u00F3n gcro\u00EDl\u00E1r amh\u00E1in a phl\u00E9ascfaidh, agus an cro\u00EDl\u00E1r f\u00E9in ag imphl\u00E9ascadh - is \u00E9 sin, ag crapadh isteach chuige f\u00E9in faoi bhr\u00FA na pl\u00E9isce agus a imtharraingthe f\u00E9in le hiomp\u00FA ina neodr\u00F3nr\u00E9alta n\u00F3 ina "@ga . . . "\u8D85\u65B0\u661F\uFF08\u3061\u3087\u3046\u3057\u3093\u305B\u3044\u3001\u82F1: supernova\u3001\u30B9\u30FC\u30D1\u30FC\u30CE\u30F4\u30A1\uFF09\u306F\u3001\u5927\u8CEA\u91CF\u306E\u6052\u661F\u3084\u8FD1\u63A5\u9023\u661F\u7CFB\u306E\u767D\u8272\u77EE\u661F\u304C\u8D77\u3053\u3059\u5927\u898F\u6A21\u306A\u7206\u767A\uFF08\u8D85\u65B0\u661F\u7206\u767A\uFF09\u306B\u3088\u3063\u3066\u8F1D\u304F\u5929\u4F53\u306E\u3053\u3068\u3002"@ja . . . . . . . . . "\u039F \u03CC\u03C1\u03BF\u03C2 \u03C5\u03C0\u03B5\u03C1\u03BA\u03B1\u03B9\u03BD\u03BF\u03C6\u03B1\u03BD\u03AE\u03C2 \u03B1\u03C3\u03C4\u03AD\u03C1\u03B1\u03C2 \u03AE \u03C3\u03BF\u03C5\u03C0\u03B5\u03C1\u03BD\u03CC\u03B2\u03B1 (supernova) \u03B1\u03BD\u03B1\u03C6\u03AD\u03C1\u03B5\u03C4\u03B1\u03B9 \u03C3\u03B5 \u03B4\u03B9\u03AC\u03C6\u03BF\u03C1\u03BF\u03C5\u03C2 \u03C4\u03CD\u03C0\u03BF\u03C5\u03C2 \u03B5\u03BA\u03C1\u03AE\u03BE\u03B5\u03C9\u03BD \u03C0\u03BF\u03C5 \u03C3\u03C5\u03BC\u03B2\u03B1\u03AF\u03BD\u03BF\u03C5\u03BD \u03BA\u03B1\u03C4\u03AC \u03C4\u03B7 \u03B4\u03B9\u03AC\u03C1\u03BA\u03B5\u03B9\u03B1 \u03C4\u03C9\u03BD \u03C4\u03B5\u03BB\u03B5\u03C5\u03C4\u03B1\u03AF\u03C9\u03BD \u03B5\u03BE\u03B5\u03BB\u03B9\u03BA\u03C4\u03B9\u03BA\u03CE\u03BD \u03C3\u03C4\u03B1\u03B4\u03AF\u03C9\u03BD \u03C4\u03B7\u03C2 \u03B6\u03C9\u03AE\u03C2 \u03C4\u03C9\u03BD \u03B1\u03C3\u03C4\u03AD\u03C1\u03C9\u03BD, \u03BA\u03B1\u03C4\u03AC \u03C4\u03B9\u03C2 \u03BF\u03C0\u03BF\u03AF\u03B5\u03C2 \u03C0\u03B1\u03C1\u03AC\u03B3\u03BF\u03BD\u03C4\u03B1\u03B9 \u03B5\u03BE\u03B1\u03B9\u03C1\u03B5\u03C4\u03B9\u03BA\u03AC \u03C6\u03C9\u03C4\u03B5\u03B9\u03BD\u03AC \u03B1\u03BD\u03C4\u03B9\u03BA\u03B5\u03AF\u03BC\u03B5\u03BD\u03B1, \u03B1\u03C0\u03BF\u03C4\u03B5\u03BB\u03BF\u03CD\u03BC\u03B5\u03BD\u03B1 \u03B1\u03C0\u03CC \u03C0\u03BB\u03AC\u03C3\u03BC\u03B1 (\u03B9\u03BF\u03BD\u03B9\u03C3\u03BC\u03AD\u03BD\u03B7 \u03CD\u03BB\u03B7) \u03BA\u03B1\u03B9 \u03C4\u03C9\u03BD \u03BF\u03C0\u03BF\u03AF\u03C9\u03BD \u03B7 \u03B1\u03C1\u03C7\u03B9\u03BA\u03AE \u03C6\u03C9\u03C4\u03B5\u03B9\u03BD\u03CC\u03C4\u03B7\u03C4\u03B1 \u03C3\u03C4\u03B7 \u03C3\u03C5\u03BD\u03AD\u03C7\u03B5\u03B9\u03B1 \u03B1\u03B4\u03C5\u03BD\u03B1\u03C4\u03AF\u03B6\u03B5\u03B9 \u03BC\u03AD\u03C7\u03C1\u03B9 \u03C4\u03BF\u03C5 \u03C3\u03B7\u03BC\u03B5\u03AF\u03BF\u03C5 \u03C4\u03B7\u03C2 \u03B1\u03C6\u03AC\u03BD\u03B5\u03B9\u03B1\u03C2 \u03BC\u03AD\u03C3\u03B1 \u03C3\u03B5 \u03BB\u03AF\u03B3\u03BF\u03C5\u03C2 \u03BC\u03AE\u03BD\u03B5\u03C2. \u0397 \u03AD\u03BA\u03C1\u03B7\u03BE\u03B7 \u03C4\u03C9\u03BD \u03B1\u03C3\u03C4\u03AD\u03C1\u03C9\u03BD \u03B5\u03AF\u03BD\u03B1\u03B9 \u03C4\u03B5\u03C1\u03B1\u03C3\u03C4\u03AF\u03C9\u03BD \u03B4\u03B9\u03B1\u03C3\u03C4\u03AC\u03C3\u03B5\u03C9\u03BD, \u03BE\u03B5\u03C0\u03B5\u03C1\u03BD\u03AC \u03C4\u03B7\u03BD \u03B5\u03BD\u03AD\u03C1\u03B3\u03B5\u03B9\u03B1 \u03C0\u03BF\u03C5 \u03B5\u03BE\u03B1\u03C0\u03BF\u03BB\u03CD\u03B5\u03C4\u03B1\u03B9 \u03B1\u03C0\u03CC \u03C4\u03BF\u03BD \u0389\u03BB\u03B9\u03BF \u03BA\u03B1\u03B9 \u03BA\u03B1\u03C4' \u03B1\u03C5\u03C4\u03CC \u03C4\u03BF\u03BD \u03C4\u03C1\u03CC\u03C0\u03BF \u00AB\u03C0\u03B5\u03B8\u03B1\u03AF\u03BD\u03BF\u03C5\u03BD\u00BB. \u0391\u03C0\u03CC \u03C4\u03B7 \u03B3\u03AE\u03B9\u03BD\u03B7 \u03B1\u03C4\u03BC\u03CC\u03C3\u03C6\u03B1\u03B9\u03C1\u03B1 \u03BA\u03B1\u03B9 \u03B3\u03B5\u03BD\u03B9\u03BA\u03AC \u03B1\u03C0\u03CC \u03C4\u03B7 \u03B3\u03B7 \u03AD\u03BD\u03B1\u03C2 \u03C3\u03BF\u03C5\u03C0\u03B5\u03C1\u03BD\u03CC\u03B2\u03B1 \u03C6\u03B1\u03AF\u03BD\u03B5\u03C4\u03B1\u03B9 \u03C3\u03B1\u03BD \u03AD\u03BD\u03B1 \u03B5\u03BE\u03B1\u03B9\u03C1\u03B5\u03C4\u03B9\u03BA\u03AC \u03C6\u03C9\u03C4\u03B5\u03B9\u03BD\u03CC \u03B1\u03C3\u03C4\u03AD\u03C1\u03B9 \u03C0\u03BF\u03C5 \u03B4\u03B5\u03BD \u03B2\u03C1\u03B9\u03C3\u03BA\u03CC\u03C4\u03B1\u03BD \u03C3\u03B5 \u03B5\u03BA\u03B5\u03AF\u03BD\u03B7 \u03C4\u03B7 \u03B8\u03AD\u03C3\u03B7 \u03C0\u03C1\u03B9\u03BD \u03BA\u03AC\u03C0\u03BF\u03B9\u03B5\u03C2 \u03CE\u03C1\u03B5\u03C2. \u039F \u03B8\u03AC\u03BD\u03B1\u03C4\u03BF\u03C2 \u03C4\u03BF\u03C5 \u03B1\u03C3\u03C4\u03B5\u03C1\u03B9\u03BF\u03CD, \u03BF \u03BB\u03B5\u03B3\u03CC\u03BC\u03B5\u03BD\u03BF\u03C2 \u03C3\u03BF\u03C5\u03C0\u03B5\u03C1\u03BD\u03CC\u03B2\u03B1, \u03B5\u03C0\u03AD\u03C1\u03C7\u03B5\u03C4\u03B1\u03B9 \u03BC\u03B5\u03C4\u03AC \u03B1\u03C0\u03CC \u03C0\u03B5\u03C1\u03AF\u03C0\u03BF\u03C5 10 \u03BC\u03B5 20 \u03B5\u03BA\u03B1\u03C4\u03BF\u03BC\u03BC\u03CD\u03C1\u03B9\u03B1 \u03AD\u03C4\u03B7."@el . "\u0421\u0432\u0435\u0440\u0445\u043D\u043E\u0432\u0430\u044F \u0437\u0432\u0435\u0437\u0434\u0430"@ru . . "Uma supernova \u00E9 uma explos\u00E3o estelar poderosa e luminosa. Este evento astron\u00F4mico transit\u00F3rio ocorre durante os \u00FAltimos est\u00E1gios evolutivos de uma estrela massiva ou quando uma an\u00E3 branca inicia uma fus\u00E3o nuclear descontrolada. O objeto original, chamado de progenitor, pode colapsar em uma estrela de n\u00EAutrons ou em um buraco negro, podendo ainda ser completamente destru\u00EDdo. O pico de luminosidade \u00F3ptica de uma supernova pode ser compar\u00E1vel ao de uma gal\u00E1xia inteira e demora v\u00E1rias semanas ou meses at\u00E9 desaparecer. As supernovas s\u00E3o mais en\u00E9rgicas do que as novas. Em latim, nova significa \"novo\", referindo-se astronomicamente ao que parece ser uma nova estrela brilhante tempor\u00E1ria. Adicionar o prefixo \"super-\" distingue as supernovas das novas comuns, que s\u00E3o muito menos luminosas. A palavra supernova foi cunhada por Walter Baade e Fritz Zwicky em 1929. A supernova mais recente diretamente observada na Via L\u00E1ctea foi a Supernova de Kepler em 1604, mas vest\u00EDgios de supernovas mais recentes j\u00E1 foram encontrados. As observa\u00E7\u00F5es de supernovas em outras gal\u00E1xias sugerem que elas ocorrem na Via L\u00E1ctea, em m\u00E9dia, cerca de tr\u00EAs vezes a cada s\u00E9culo. Essas supernovas seriam quase certamente observ\u00E1veis com telesc\u00F3pios astron\u00F4micos modernos. A mais recente supernova vis\u00EDvel a olho nu foi a SN 1987A, cuja progenitora era uma estrela supergigante azul localizada na Grande Nuvem de Magalh\u00E3es, uma gal\u00E1xia sat\u00E9lite da Via L\u00E1ctea. Estudos te\u00F3ricos indicam que a maioria das supernovas s\u00E3o desencadeadas por um de dois mecanismos b\u00E1sicos: a s\u00FAbita re-igni\u00E7\u00E3o da fus\u00E3o nuclear em uma estrela degenerada, como uma an\u00E3 branca, ou o colapso gravitacional repentino do n\u00FAcleo de uma estrela massiva. Na primeira classe de eventos, a temperatura do objeto \u00E9 elevada o suficiente para desencadear uma avalanche t\u00E9rmica, desestruturando completamente a estrela. As poss\u00EDveis causas s\u00E3o um ac\u00FAmulo de material de uma companheira bin\u00E1ria por meio de uma acre\u00E7\u00E3o ou fus\u00E3o estelar. No caso da estrela massiva, o n\u00FAcleo de uma estrela massiva pode sofrer um colapso repentino, liberando energia potencial gravitacional como uma supernova. Embora algumas supernovas observadas sejam mais complexas do que essas duas teorias simplificadas, a mec\u00E2nica astrof\u00EDsica foi estabelecida e aceita pela maioria dos astr\u00F4nomos h\u00E1 algum tempo. As supernovas podem expelir v\u00E1rias massas solares de material a velocidades que chegam a at\u00E9 v\u00E1rios por cento da velocidade da luz. Isso impulsiona uma onda de choque em expans\u00E3o no meio interestelar circundante, varrendo uma camada de g\u00E1s e poeira em expans\u00E3o observada como um remanescente de supernova. As supernovas s\u00E3o uma importante fonte de elementos no meio interestelar, do oxig\u00EAnio ao rub\u00EDdio. As ondas de choque em expans\u00E3o das supernovas podem desencadear a forma\u00E7\u00E3o de novas estrelas. Remanescentes de supernovas podem ser uma importante fonte de raios c\u00F3smicos. As supernovas podem produzir ondas gravitacionais, embora, at\u00E9 agora, as ondas gravitacionais tenham sido detectadas apenas a partir da fus\u00E3o de buracos negros e estrelas de n\u00EAutrons."@pt . . . "Supernova"@nl . . . . "Une supernova est l'ensemble des ph\u00E9nom\u00E8nes qui r\u00E9sultent de l'implosion d'une \u00E9toile en fin de vie, notamment une gigantesque explosion qui s'accompagne d'une augmentation br\u00E8ve mais fantastiquement grande de sa luminosit\u00E9. Vue depuis la Terre, une supernova appara\u00EEt donc souvent comme une \u00E9toile nouvelle, alors qu'elle correspond en r\u00E9alit\u00E9 \u00E0 la disparition d'une \u00E9toile. Aucune supernova n'a \u00E9t\u00E9 observ\u00E9e dans notre galaxie, la Voie lact\u00E9e, depuis l'invention du t\u00E9lescope. La plus rapproch\u00E9e observ\u00E9e depuis est SN 1987A, survenue dans une galaxie voisine, le Grand Nuage de Magellan."@fr . . "Una supernova \u00E9s una explosi\u00F3 estel\u00B7lar tremendament energ\u00E8tica i lluminosa. Es tracta d'un esdeveniment astron\u00F2mic transitori que correspon a les fases finals de la vida d'un estel massiu o l'embalament de la fusi\u00F3 nuclear en un nan blanc. L'objecte original, el progenitor, es col\u00B7lapsa per esdevenir un estel de neutrons o un forat negre o \u00E9s destru\u00EFt. Una supernova pot arribar a brillar tant com una gal\u00E0xia sencera abans d'anar-se apagant en un per\u00EDode de setmanes o mesos."@ca . . . . . . . . . . . "Olln\u00F3va"@ga . . . . . . . . . . . . . . . . . . "Supernova"@ca . "Supernova"@it . . . . . . . . . . . "right"@en . . . . . . "\u8D85\u65B0\u661F\uFF08\u3061\u3087\u3046\u3057\u3093\u305B\u3044\u3001\u82F1: supernova\u3001\u30B9\u30FC\u30D1\u30FC\u30CE\u30F4\u30A1\uFF09\u306F\u3001\u5927\u8CEA\u91CF\u306E\u6052\u661F\u3084\u8FD1\u63A5\u9023\u661F\u7CFB\u306E\u767D\u8272\u77EE\u661F\u304C\u8D77\u3053\u3059\u5927\u898F\u6A21\u306A\u7206\u767A\uFF08\u8D85\u65B0\u661F\u7206\u767A\uFF09\u306B\u3088\u3063\u3066\u8F1D\u304F\u5929\u4F53\u306E\u3053\u3068\u3002"@ja . . "Supernowa"@pl . . . . . .