![\"Mnohem](\"https:\/\/www.osel.cz\/popisek.php?popisek=44300&img=best-image-of-alpha-centauri-a-and-b.jpeg\" "\\"Mnohem")
<\/a><\/p>\nMnohem m\u00e9n\u011b extr\u00e9mn\u00ed dvojhv\u011bzda pro ilustraci. Kredit: ESA\/Hubble & NASA, Wikimedia Commons, CC BY-SA 4.0.<\/p>\n
V\u011bdci se u\u017e dlouho sna\u017e\u00ed vystopovat zdroje nejv\u00edce energetick\u00fdch \u010d\u00e1stic v na\u0161\u00ed galaxii, tvrd\u00e9ho kosmick\u00e9ho z\u00e1\u0159en\u00ed, kter\u00e9 nese energie dalece p\u0159esahuj\u00edc\u00ed mo\u017enosti na\u0161ich urychlova\u010d\u016f. Vysokohorsk\u00e1 gamaobservato\u0159 LHAASO (Large High Altitude Air Shower Observatory) narazila na jeden hodn\u011b exotick\u00fd zdroj, kter\u00fd v\u011bdci ne\u010dekali.<\/p>\n
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Observato\u0159 LHAASO pod sn\u011bhem. Kredit: LHAASO Team \/ CAS.<\/p>\n LHAASO, kter\u00e1 pracuje ve v\u00fd\u0161ce kolem 4\u00a0410 metr\u016f nad mo\u0159em, p\u0159istihla dvojhv\u011bzdu s\u00a0krkolomn\u00fdm n\u00e1zvem LS I +61\u00b0 303 p\u0159i emisi gama z\u00e1\u0159en\u00ed s energiemi nad 100 teraelektronvolt\u016f (TeV). Pro srovn\u00e1n\u00ed, jde o v\u00edce ne\u017e patn\u00e1ctin\u00e1sobek energie protonu v nejv\u00fdkonn\u011bj\u0161\u00edm lidsk\u00e9m sr\u00e1\u017ee\u010di LHC, kter\u00e1 se pohybuje kolem 6,5 TeV (ve sr\u00e1\u017ek\u00e1ch je to tedy dvojn\u00e1sobek). Je to poprv\u00e9 co byla takto extr\u00e9mn\u00ed emise potvrzena u gama-dvojhv\u011bzdy (gamma ray binary).<\/p>\n \u00a0<\/p>\n Gama dvojhv\u011bzda (ilustrace). Kredit: NASA\u2019s Goddard Space Flight Center.<\/p>\n \u00a0<\/p>\n Detekovat vysokoenergetick\u00e9 gama z\u00e1\u0159en\u00ed na Zemi je velmi obt\u00ed\u017en\u00e9. Vlastn\u011b je to nemo\u017en\u00e9. Gama z\u00e1\u0159en\u00ed nepronikne a\u017e na zemsk\u00fd povrch. Spou\u0161t\u00ed ale sekund\u00e1rn\u00ed spr\u0161ky z\u00e1\u0159en\u00ed (air shower), kter\u00e9 detekuje observato\u0159 LHAASO. Z\u00a0pozorov\u00e1n\u00ed spr\u0161ek pak lze rekonstruovat energii, p\u0159\u00edpadn\u011b i p\u016fvod vysokoenergetick\u00e9ho fotonu gama z\u00e1\u0159en\u00ed, kter\u00fd spr\u0161ku vyvolal.<\/p>\n \u00a0<\/p>\n Syst\u00e9m LS I +61\u00b0 303 je doopravdy extr\u00e9mn\u00ed nebo sp\u00ed\u0161 \u0161\u00edlen\u00fd. Je to masivn\u00ed hv\u011bzda, podstatn\u011b hmotn\u011bj\u0161\u00ed ne\u017e Slunce, jej\u00edm\u017e partnerem je kompaktn\u00ed objekt, pravd\u011bpodobn\u011b neutronov\u00e1 hv\u011bzda nebo \u010dern\u00e1 d\u00edra. Jsou tak t\u011bsn\u011b u sebe, \u017ee se ob\u011bhnou jednou za 26,5 dne.<\/p>\n Pozorovan\u00e9 parametry t\u00e9to dvojhv\u011bzdy ukazuj\u00ed, \u017ee kolem sebe vytvo\u0159ila velmi dramatick\u00e9 prost\u0159ed\u00ed, kter\u00e9 se neust\u00e1le vyv\u00edj\u00ed, a\u0165 jde o magnetick\u00e1 pole, hustotu \u010d\u00e1stic nebo dal\u0161\u00ed parametry. Je to jako extr\u00e9mn\u00ed kosmick\u00fd reaktor, kter\u00fd ka\u017ed\u00fdch p\u00e1r dn\u00ed m\u011bn\u00ed svou fyziku. Podle v\u011bdc\u016f jsou tam ve h\u0159e sp\u00ed\u0161e protony a t\u011b\u017e\u0161\u00ed \u010d\u00e1stice, kter\u00e9 generuj\u00ed vysokoenergetick\u00e9 gama z\u00e1\u0159en\u00ed p\u0159i sv\u00fdch interakc\u00edch.<\/p>\n P\u0159es tyto poznatky zat\u00edm nen\u00ed \u00fapln\u011b jasn\u00e9, jak\u00fd mechanismus urychluje \u010d\u00e1stice ve fyzik\u00e1ln\u00edm pekle dvojhv\u011bzdy LS I +61\u00b0 303. Je\u0161t\u011b budou nutn\u00e1 dal\u0161\u00ed pozorov\u00e1n\u00ed, a nejen v oblasti gama z\u00e1\u0159en\u00ed, abychom z\u00edskali p\u0159edstavu, jak to tam vlastn\u011b funguje.<\/p>\n \u00a0<\/p>\n Video: World’s most sensitive cosmic-ray observatory: A look inside LHAASO<\/p>\n \n \u00a0<\/p>\n Literatura<\/p>\n<\/a><\/p>\n<\/a><\/p>\n