{"id":5414,"date":"2022-01-25T09:13:00","date_gmt":"2022-01-25T08:13:00","guid":{"rendered":"https:\/\/www.christian-doppler.net\/?post_type=thema&p=5414"},"modified":"2022-01-26T17:00:42","modified_gmt":"2022-01-26T16:00:42","slug":"astronomie","status":"publish","type":"thema","link":"https:\/\/www.christian-doppler.net\/cs\/thema\/astronomie\/","title":{"rendered":"Astronomie"},"content":{"rendered":"\n
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Dne 25. kv\u011btna 1842 p\u0159edstavil Christian Doppler Kr\u00e1lovsk\u00e9 \u010desk\u00e9 spole\u010dnosti nauk sv\u016fj spis \u201eO barevn\u00e9m sv\u011btle dvojhv\u011bzd\u201c a proslavil se tak po cel\u00e9m sv\u011bt\u011b. <\/p>\n\n\n\n

Doppler\u016fv jev a barevn\u00e9 hv\u011bzdy<\/strong><\/strong><\/h2>\n\n\n\n

Fyzici se ji\u017e tehdy nau\u010dili m\u011b\u0159it frekvenci sv\u011btla (elektromagnetick\u00e9 vln\u011bn\u00ed) a zjistili, \u017ee \u010derven\u00e9 sv\u011btlo m\u00e1 men\u0161\u00ed frekvenci (od 390 THz, tj. 390 s 12 nulami za vte\u0159inu) ne\u017e modr\u00e9 sv\u011btlo (a\u017e 770 THz).<\/p>\n\n\n\n

\u010c\u00edm rychleji se od n\u00e1s hv\u011bzda vzdaluje, t\u00edm v\u00edce se jej\u00ed sv\u011btlo posunuje do ni\u017e\u0161\u00ed frekvence \u010dili do spektra rud\u00e9ho sv\u011btla. Sv\u011btlo ur\u010dit\u00fdch element\u016f m\u00e1 p\u0159itom ni\u017e\u0161\u00ed frekvence ne\u017e u n\u00e1s nebo u bli\u017e\u0161\u00edch hv\u011bzd, jako i u mal\u00e9 \u017elut\u00e9 hv\u011bzdy Slunce.<\/p>\n\n\n\n

Velkou pomoc\u00ed p\u0159i tomto zkoum\u00e1n\u00ed bylo, \u017ee n\u011bkter\u00e9 l\u00e1tky vytv\u00e1\u0159\u00ed (nebo pohlcuj\u00ed) zcela ur\u010ditou barvu (frekvenci). Pomoc\u00ed optick\u00e9ho hranolu vid\u00edme spektr\u00e1ln\u00ed \u010d\u00e1ry (disperze sv\u011btla).<\/p>\n\n\n\n

U dvojhv\u011bzd krou\u017e\u00ed pov\u011bt\u0161inou jedna men\u0161\u00ed a jedna v\u011bt\u0161\u00ed hv\u011bzda kolem spole\u010dn\u00e9ho t\u011b\u017ei\u0161t\u011b. Jestli\u017ee je jejich dr\u00e1ha hv\u011bzdy rovnob\u011b\u017en\u00e1 se zorn\u00fdm paprskem pozorovatele ze Zem\u011b, zakr\u00fdv\u00e1 v\u011bt\u0161\u00ed hv\u011bzda pravideln\u011b hv\u011bzdu men\u0161\u00ed. Rychlost obou hv\u011bzd lze velmi p\u0159esn\u011b ur\u010dit v okam\u017eiku jejich nejv\u011bt\u0161\u00edho z\u0159ejm\u00e9ho rozestupu za pomoci dopplerovsk\u00e9ho posunu. I p\u0159es tehdej\u0161\u00ed nedostate\u010dn\u00e9 znalosti o barevnosti r\u016fzn\u00fdch druh\u016f hv\u011bzd se Dopplerovi poda\u0159ilo vytvo\u0159it pro astronomii u\u017eite\u010dnou teorii, by\u0165 byla jej\u00ed spr\u00e1vnost prok\u00e1z\u00e1na a\u017e s odstupem \u010dasu.     <\/p>\n\n\n\n

Astronomie dnes: mo\u017enosti Dopplerova jevu<\/strong><\/strong><\/h2>\n\n\n\n

Dnes je pomoc\u00ed Dopplerova jevu mo\u017en\u00e9 nejenom vypo\u010d\u00edtat rychlost hv\u011bzd a galaxi\u00ed v pom\u011bru k n\u00e1m, n\u00fdbr\u017e tak\u00e9 jejich vzd\u00e1lenosti, dobu trv\u00e1n\u00ed rotace, rychlost vzniku supernov a mnoho dal\u0161\u00edho. T\u00e9\u017e v\u00fdzkum rentgenov\u00fdch hv\u011bzd je mo\u017en\u00fd d\u00edky Dopplerovu jevu. <\/p>\n\n\n\n

Bez objev\u016f Christiana Dopplera bychom si v\u016fbec neum\u011bli p\u0159edstavit modern\u00ed astronomii, vlastn\u011b by ani nebyla mo\u017en\u00e1.<\/p>\n<\/div>\n\n\n\n

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Dal\u0161\u00ed odkazy<\/strong><\/h2>\n\n\n\n

Astronomie na Wikipedii<\/a><\/p>\n<\/div><\/div><\/div><\/div><\/div><\/div>\n<\/div>\n<\/div>\n