[{"@context":"https:\/\/schema.org\/","@type":"Article","@id":"https:\/\/www.zpraku.cz\/slunecni-soustava-venuse\/#Article","mainEntityOfPage":"https:\/\/www.zpraku.cz\/slunecni-soustava-venuse\/","headline":"Slune\u010dn\u00ed soustava \u2013 Venu\u0161e","name":"Slune\u010dn\u00ed soustava \u2013 Venu\u0161e","description":"Rozd\u00edl mezi na\u0161\u00ed planetou a Venu\u0161\u00ed je hlavn\u011b v j\u00e1dru, kter\u00e9 u Venu\u0161e nen\u00ed tvo\u0159eno dv\u011bma \u010d\u00e1stmi (tekutou a pevnou). Proto\u017ee m\u00e1 Venu\u0161e velmi slab\u00e9 magnetick\u00e9 pole, jde z\u0159ejm\u011b o velk\u00e9 a pevn\u00e9 kovov\u00e9 j\u00e1dro, kter\u00e9 je s nejv\u011bt\u0161\u00ed pravd\u011bpodobnost\u00ed tvo\u0159eno \u017eelezem a niklem. K\u016fra planety Venu\u0161e je relativn\u011b tenk\u00e1 – jej\u00ed hloubka je cca 50 km.  […]","datePublished":"2020-03-22","dateModified":"2023-05-15","author":{"@type":"Person","@id":"https:\/\/www.zpraku.cz\/author\/#Person","name":"","url":"https:\/\/www.zpraku.cz\/author\/","identifier":1,"image":{"@type":"ImageObject","@id":"https:\/\/secure.gravatar.com\/avatar\/9cae764794acc12213aa530e21558ed2bd96c03f91e0c3ad21cc1905765be658?s=96&d=mm&r=g","url":"https:\/\/secure.gravatar.com\/avatar\/9cae764794acc12213aa530e21558ed2bd96c03f91e0c3ad21cc1905765be658?s=96&d=mm&r=g","height":96,"width":96}},"publisher":{"@type":"Organization","name":"zpraku.cz","logo":{"@type":"ImageObject","@id":"\/logo.png","url":"\/logo.png","width":600,"height":60}},"image":{"@type":"ImageObject","@id":"https:\/\/www.zpraku.cz\/wp-content\/uploads\/img_a372664_w3723_t1584085035.png","url":"https:\/\/www.zpraku.cz\/wp-content\/uploads\/img_a372664_w3723_t1584085035.png","height":0,"width":0},"url":"https:\/\/www.zpraku.cz\/slunecni-soustava-venuse\/","about":["V\u011bda"],"wordCount":408,"articleBody":"Rozd\u00edl mezi na\u0161\u00ed planetou a Venu\u0161\u00ed je hlavn\u011b v j\u00e1dru, kter\u00e9 u Venu\u0161e nen\u00ed tvo\u0159eno dv\u011bma \u010d\u00e1stmi (tekutou a pevnou). Proto\u017ee m\u00e1 Venu\u0161e velmi slab\u00e9 magnetick\u00e9 pole, jde z\u0159ejm\u011b o velk\u00e9 a pevn\u00e9 kovov\u00e9 j\u00e1dro, kter\u00e9 je s nejv\u011bt\u0161\u00ed pravd\u011bpodobnost\u00ed tvo\u0159eno \u017eelezem a niklem.K\u016fra planety Venu\u0161e je relativn\u011b tenk\u00e1 – jej\u00ed hloubka je cca 50 km.  Asi 10 % planet\u00e1rn\u00edho povrchu je pokryto poho\u0159\u00edmi, kter\u00e1 jsou vy\u0161\u0161\u00ed ne\u017e 10 kilometr\u016f, 10 % tvo\u0159\u00ed poho\u0159\u00ed, jejich\u017e v\u00fd\u0161ka dosahuje od 2 do 10 km. Zbytek povrchu tvo\u0159\u00ed n\u00ed\u017einn\u00e9 planiny. V\u011bk nejstar\u0161\u00edch \u00fatvar\u016f byl odhadnut na 500 milion\u016f let. Venu\u0161e tedy byla je\u0161t\u011b „ v ned\u00e1vnu“ geologicky \u010dinn\u00e1; radarov\u00e9 fotografie ukazuj\u00ed n\u011bkter\u00e9 vyhasl\u00e9 sopky, vulkanick\u00e9 \u00fatvary zvan\u00e9 kruhov\u00e9 d\u00f3my, kter\u00e9 se podobaj\u00ed velk\u00fdm puch\u00fd\u0159\u016fm a vznikly tak, \u017ee l\u00e1va p\u0159i proniknut\u00ed na povrch vytvo\u0159ila vypoukl\u00e9 bochn\u00edkov\u00e9 kopce, kter\u00e9 se p\u0159i chladnut\u00ed smr\u0161\u0165ovaly a popraskaly.  Jin\u00e9 vulkanick\u00e9 \u00fatvary – kruhovit\u00e9 Corony – maj\u00ed pr\u016fm\u011br i 200 kilometr\u016f a sv\u011bd\u010d\u00ed o n\u011bkdej\u0161\u00ed,  intenz\u00edvn\u00ed sope\u010dn\u00e9 \u010dinnosti. Kolem t\u011bch nejv\u011bt\u0161\u00edch vrchol\u016f Venu\u0161e (nap\u0159. Maat Mons) je na sn\u00edmc\u00edch vid\u011bt, jak se \u017ehav\u00e1 l\u00e1va rozt\u00e9kala stovky kilometr\u016f po pl\u00e1n\u00edch a p\u0159i chladnut\u00ed po sob\u011b zanech\u00e1vala typick\u00fd povrch. N\u011bkter\u00e9 oblasti Venu\u0161e mohou b\u00fdt vulkanicky aktivn\u00ed doposud.Mezi k\u016frou a j\u00e1drem se nach\u00e1z\u00ed pevn\u00fd silik\u00e1tov\u00fd pl\u00e1\u0161\u0165, jen\u017e sah\u00e1 do hloubky asi 3000 kilometr\u016f.Povrch Venu\u0161e neust\u00e1le hal\u00ed atmosf\u00e9ra, tvo\u0159en\u00e1 oxidem uhli\u010dit\u00fdm a mraky kyseliny s\u00edrov\u00e9. Tohle jedovat\u00e9 prost\u0159ed\u00ed p\u016fsob\u00ed na povrch planety obrovsk\u00fdm tlakem (podobn\u00fdm jak\u00fd by byl na Zemi na dn\u011b jezera, kter\u00e9 je hlubok\u00e9 900 metr\u016f). Nav\u00edc atmosf\u00e9ra funguje jako \u017ehav\u00fd poklop planety – p\u0159esto\u017ee je Venu\u0161e od Slunce vzd\u00e1lena mnohem d\u00e1l ne\u017e Merkur, je jej\u00ed teplota vy\u0161\u0161\u00ed (pr\u016fm\u011brn\u00e1 povrchov\u00e1 teplota \u010din\u00ed 480oC a kovy jako c\u00edn a olovo by se tam snadno roztavily); je to d\u016fsledek sklen\u00edkov\u00e9ho efektu, kter\u00fd zp\u016fsobuje oxid uhli\u010dit\u00fd.Povrch planety Venu\u0161e byl zmapov\u00e1n v roce 1989 americkou sondou Magellan, a to pomoc\u00ed radaru, kter\u00fd byl schopen proniknout jej\u00edmi mra\u010dny.Venu\u0161e nem\u00e1 \u017e\u00e1dn\u00e9 ob\u011b\u017enice.                                                                                                                                                                                                                                                                                                                                                                                        4.7\/5 - (8 votes)        "},{"@context":"https:\/\/schema.org\/","@type":"BreadcrumbList","itemListElement":[{"@type":"ListItem","position":1,"name":"Slune\u010dn\u00ed soustava \u2013 Venu\u0161e","item":"https:\/\/www.zpraku.cz\/slunecni-soustava-venuse\/#breadcrumbitem"}]}]