Bir optik sistemin odak uzakl\u0131\u011f\u0131, \u0131\u015f\u0131\u011f\u0131n mercekten ge\u00e7ip k\u0131r\u0131ld\u0131\u011f\u0131 veya \u00e7ukur aynadan yans\u0131d\u0131ktan sonra k\u0131r\u0131l\u0131p, ok\u00fclerde resim olu\u015fturana kadar ge\u00e7ti\u011fi yolun uzunlu\u011fudur.<\/p>\n\n\n\n
<\/p>\n\n\n\n
ODAK ORANI NED\u0130R ?<\/strong> <\/p>\n\n\n\n Teleskoplarda ve objektiflerde, kullan\u0131m k\u0131lavuzlar\u0131nda ya da t\u00fcplerinin \u00fczerlerinde, \u00f6rne\u011fin 1000mm f\/11 D=90mm F=1000mm \u015feklinde bir tak\u0131m rakamlar\u0131n yer ald\u0131\u011f\u0131n\u0131 g\u00f6rm\u00fc\u015fs\u00fcn\u00fczd\u00fcr. <\/p>\n\n\n\n Bu \u00f6rnekteki tan\u0131m\u0131n anlam\u0131 \u015fudur:<\/p>\n\n\n\n D: Objektif (ayna ya da mercek) \u00e7ap\u0131 (diameter) = 90 mm <\/p>\n\n\n\n F: Odak uzakl\u0131\u011f\u0131 (focal length) = 1000 mm <\/p>\n\n\n\n f\/: Odak oran\u0131 : Odak uzakl\u0131\u011f\u0131 \/ objektif \u00e7ap\u0131 = 1000 \/ 90 = 11<\/p>\n\n\n\n <\/p>\n\n\n\n B\u00dcY\u00dcTME G\u00dcC\u00dc NED\u0130R ?<\/strong><\/p>\n\n\n\n OPT\u0130K TELESKOP T\u00dcRLER\u0130<\/strong><\/p>\n\n\n\n -Mercekli teleskoplar<\/p>\n\n\n\n -Aynal\u0131 teleskoplar<\/p>\n\n\n\n -Hem mercekli hem aynal\u0131 teleskoplar<\/p>\n\n\n\n Mercekli Teleskoplar<\/strong><\/p>\n\n\n\n Mercekli teleskoplarda \u0131\u015f\u0131k cam i\u00e7inden ge\u00e7erken k\u0131r\u0131l\u0131r ve odaklan\u0131r. Ancak her renk farkl\u0131 uzakl\u0131klarda odakland\u0131\u011f\u0131ndan renksel sap\u0131n\u00e7 ( aberasyon ) meydana gelir. Bunu engellemek i\u00e7in \u201c Flint \u201c ve \u201c Crown \u201c isimli \u00f6zel camlardan olu\u015fan mercekler yap\u0131l\u0131r. Normal cam gelen \u0131\u015f\u0131\u011f\u0131n % 10\u2019 unu geri yans\u0131t\u0131r, bundan dolay\u0131 merceklerin y\u00fczeylerine kaplama yap\u0131l\u0131r. Bu kaplama sayesinde gelen \u0131\u015f\u0131\u011f\u0131n % 1\u2019 i geri yans\u0131r, bunlara \u201c Apochromatic \u201c mercekler denir.<\/p>\n\n\n\n <\/p>\n\n\n\n Aynal\u0131 Teleskoplar<\/strong><\/p>\n\n\n\n Newton tipi teleskop amat\u00f6r astromlar i\u00e7in en kolay ve muhtemelen en pop\u00fcler teleskop tipidir. Genellikle \u00e7o\u011fu ev yap\u0131m\u0131 amat\u00f6r ayg\u0131tlar\u0131d\u0131r. Asl\u0131nda Newton tipi teleskop performanslar\u0131 \u00f6l\u00e7\u00fclm\u00fc\u015f di\u011fer teleskoplara g\u00f6re daha pratiktir. Newton tipi optik sistem parabolik birincil ayna ve bu aynan\u0131n y\u00f6nlendirdi\u011fi konik \u0131\u015f\u0131n demetinin i\u00e7inde kalan d\u00fcz ikincil aynadan olu\u015fmaktad\u0131r.<\/p>\n\n\n\n Bu ayg\u0131t\u0131n karakteristi\u011fi nedir?<\/p>\n\n\n\n Odak oran\u0131 genellikle f\/4 ve f\/12 aras\u0131nda de\u011fi\u015fir. H\u0131zl\u0131 b\u00fcy\u00fctme optik eksenin d\u0131\u015f\u0131nda kuyruk sa\u00e7\u0131lmas\u0131n\u0131 ( coma ) artt\u0131raca\u011f\u0131ndan f\/4 kullan\u0131\u015fl\u0131 en d\u00fc\u015f\u00fck limittir. f\/12 ise ayg\u0131t\u0131n uzunlu\u011fu \u00e7ok fazla olaca\u011f\u0131ndan en \u00fcst limittir. G\u00f6ky\u00fcz\u00fc foto\u011fraf\u00e7\u0131l\u0131\u011f\u0131 ve derin uzay g\u00f6zlemi i\u00e7in esas olan h\u0131zl\u0131l\u0131k ( f\/4 – f\/6 aral\u0131\u011f\u0131 ) uygun iken Ay ve gezegen g\u00f6zlemleri i\u00e7in esas olan yava\u015fl\u0131l\u0131k ( f\/7 – f\/12 aral\u0131\u011f\u0131 ) d\u00fc\u015f\u00fcn\u00fclebilir.<\/p>\n\n\n\n Birincil aynan\u0131n merkezi diagonal ( ikincil ayna ) taraf\u0131ndan engellenir. Bu eleman odak d\u00fczlemine gereken b\u00f6lgeyi ayd\u0131nlatabilecek kadar b\u00fcy\u00fck olmal\u0131d\u0131r. Bununla birlikte gerekenden daha b\u00fcy\u00fck olmamal\u0131d\u0131r, \u00e7\u00fcnk\u00fc bu sistemin optik performans\u0131n\u0131 azalt\u0131r.<\/p>\n\n\n\n Nispeten k\u00fc\u00e7\u00fck ve yava\u015f Newton teleskobun birincil aynas\u0131n\u0131n parabolik olmas\u0131na gerek yoktur. Her ne kadar bug\u00fcn bir \u00e7ok Newton tipi parabolik ayna kullan\u0131larak yap\u0131l\u0131yor olsa da, Newton tipinin karakteristik incelemesine k\u00fcresel ayna ile ba\u015flayaca\u011f\u0131z. \u00c7\u00fcnk\u00fc k\u00fcresel ayna yapmak olduk\u00e7a kolayd\u0131r, bu t\u00fcm teleskoplar\u0131n en kolay\u0131 ve amat\u00f6rlerin ilk tercihidir.<\/p>\n\n\n\n Bir k\u00fcresel aynada e\u015f-eksenli \u0131\u015f\u0131nlar F ( odak noktas\u0131 ) noktas\u0131nda kesi\u015fir. Eksen oda\u011f\u0131ndan daha uzak noktalar aynaya do\u011fru yakla\u015ft\u0131k\u00e7a g\u00f6r\u00fcnt\u00fc k\u00fcresel sap\u0131n\u00e7tan daha \u00e7ok etkilenmeye ba\u015flar. Yak\u0131nsak \u0131\u015f\u0131n demeti H1 d\u00fczleminde en k\u00fc\u00e7\u00fck kesite uzan\u0131r. Bununla beraber H1 ile F aras\u0131nda bir yerde H2 yak\u0131nsak \u0131\u015f\u0131n demetinin yo\u011funlu\u011fu olduk\u00e7a y\u00fcksektir. Bu parlak merkez herhangi bir odaktan daha keskin g\u00f6r\u00fcnt\u00fcler verir.<\/p>\n\n\n\n <\/p>\n\n\n\n Katadiyoptrik (Hem Mercekli Hem Aynal\u0131 ) Teleskoplar<\/strong><\/p>\n\n\n\n Katadiyoptrik teleskoplar\u0131n tan\u0131m\u0131n\u0131 yaparsak, optik d\u00fczene\u011finde hem mercek hem de ayna kullan\u0131lan teleskoplardan bahsetmi\u015f oluruz. Bu t\u00fcrdeki teleskoplar optik d\u00fczenekleri sayesinde hem Newton t\u00fcr\u00fc teleskoplardaki coma ( g\u00f6r\u00fcnt\u00fcn\u00fcn tek bir odakta toplanmamas\u0131 ) sorununu, hem de mercekli teleskoplardaki renk sapmas\u0131n\u0131 ( \u0131\u015f\u0131\u011f\u0131n k\u0131r\u0131l\u0131rken de\u011fi\u015fik dalga boylar\u0131nda ayr\u0131\u015fmas\u0131 ) \u00f6nledi\u011fi i\u00e7in tercih edilirler. Ayr\u0131ca, \u0131\u015f\u0131k demeti teleskop t\u00fcp\u00fcn\u00fcn i\u00e7inde \u00fc\u00e7 kere yans\u0131d\u0131\u011f\u0131ndan t\u00fcp boylar\u0131 da ayn\u0131 odak uzakl\u0131\u011f\u0131na sahip di\u011fer teleskoplara g\u00f6re daha k\u0131sa olur.<\/p>\n\n\n\n B\u00fct\u00fcn bu olumlu y\u00f6nlerine kar\u015f\u0131n baz\u0131 kusurlar\u0131 da vard\u0131r. Birincisi, g\u00f6r\u00fc\u015f a\u00e7\u0131lar\u0131n\u0131n daha dar olmas\u0131d\u0131r ( Schmidt-Newtonian t\u00fcr\u00fc d\u0131\u015f\u0131ndakiler ). \u0130kinci kusur, ikincil aynalar\u0131n ( \u00f6zellikle Schmidt Cassegrain t\u00fcr\u00fcndekilerin ) b\u00fcy\u00fck olmas\u0131ndan dolay\u0131 merkezi \u00f6rtme oranlar\u0131n\u0131n fazlal\u0131\u011f\u0131 ( cm2 cinsinden yakla\u015f\u0131k % 30 lar d\u00fczeyinde ) ve b\u00f6ylece de g\u00f6r\u00fcnt\u00fcdeki kar\u015f\u0131tl\u0131\u011f\u0131 ( contrast ) d\u00fc\u015f\u00fcrmeleridir.<\/p>\n\n\n\n Katadiyoptrik teleskoplarda birincil ayna k\u00fcreseldir. Teleskobun \u00f6n\u00fcne yerle\u015ftirilen \u00f6zel \u015fekilli mercek bu k\u00fcresel aynan\u0131n optik kusurlar\u0131n\u0131 ( en \u00f6nemlisi k\u00fcresel sap\u0131n\u00e7 \/ yans\u0131yan \u0131\u015f\u0131nlar\u0131n tek bir odakta toplanmamas\u0131 ) gidermekte kullan\u0131l\u0131r. <\/p>\n\n\n\n Schmidt Cassegrain ( SC ) <\/strong>t\u00fcr teleskoplarda d\u00fczeltici merce\u011fin karma\u015f\u0131k bie \u015fekli vard\u0131r. ( Aspheric ). Maksutov Cassegrain <\/strong>( Maksutov ) t\u00fcr\u00fc teleskoplar\u0131n \u00f6nlerinde yer alan kusur d\u00fczeltici merce\u011fin \u00e7ukurlu\u011fu fazla olup, yine k\u00fcresel bi\u00e7imdedir. Maksutov teleskoplar amat\u00f6r ya da profesyonel olsun bir \u00e7ok kullan\u0131c\u0131ya g\u00f6re SC teleskoplardan \u00e7ok daha iyi bir optik d\u00fczene\u011fe sahip olarak kabul edilmektedir. Bunun i\u00e7in en \u00f6nde gelen neden ikincil aynalar\u0131n\u0131n SC\u2019 lere g\u00f6re daha k\u00fc\u00e7\u00fck olmas\u0131 ve bu \u015fekilde g\u00f6r\u00fcnt\u00fc kar\u015f\u0131tl\u0131\u011f\u0131n\u0131 artt\u0131rmas\u0131d\u0131r. Pek \u00e7ok amat\u00f6re g\u00f6re Maksutavlar gezegen g\u00f6zlemlerinde mercekli teleskoplardan daha iyi sonu\u00e7lar verebilmektedir. Maksutovlar\u0131n ikincil aynalar\u0131 d\u00fczeltici merce\u011fin i\u00e7 y\u00fczeyine s\u0131rlanm\u0131\u015ft\u0131r. SC\u2019 lerde ise ikincil ayna \u00f6n cama ayr\u0131ca tutturulur ve \u00e7ap\u0131 daha b\u00fcy\u00fckt\u00fcr.<\/p>\n\n\n\n Ritchey – Chretien <\/strong>( RC ) t\u00fcr\u00fc teleskoplar\u0131n en \u00f6nemli fark\u0131, hem birincil hem de ikincil aynalar\u0131n\u0131n y\u00fczey \u015feklinin hiperbolik olmas\u0131d\u0131r. Optik kusurlar\u0131n bu \u015fekilde daha iyi d\u00fczeltildi\u011fi ileri s\u00fcr\u00fclmektedir.<\/p>\n\n\n\n Schmidt – Newtonian <\/strong>( SN ) t\u00fcr\u00fc teleskoplarda birincil ayna yine k\u00fcresel olup, odak uzakl\u0131\u011f\u0131 ayn\u0131 \u00e7aptaki Newton t\u00fcr\u00fc teleskoplara g\u00f6re daha azd\u0131r. Bu da t\u00fcp boylar\u0131n\u0131 daha k\u0131sa ve g\u00f6r\u00fc\u015f a\u00e7\u0131lar\u0131n\u0131n daha geni\u015f olmas\u0131n\u0131 sa\u011flamaktad\u0131r. Bu sayede SN teleskoplarda elde edilen g\u00f6r\u00fcnt\u00fc daha parlak olmaktad\u0131r. Bu nedenle genelde astrofoto\u011frafi i\u00e7in kullan\u0131\u015fl\u0131d\u0131rlar. K\u0131sa odakl\u0131 k\u00fcresel aynalar\u0131n yap\u0131m\u0131 nispeten daha kolayd\u0131r. Aynan\u0131n hem k\u00fcresel hem de k\u0131sa odak uzakl\u0131kl\u0131 olmas\u0131ndan kaynaklanan optik kusurlar, yine teleskop t\u00fcp\u00fcn\u00fcn \u00f6n\u00fcne yerle\u015ftirilen Schmidt merce\u011fi ile d\u00fczeltilir.<\/p>\n\n\n\n Teleskop t\u00fcrleri a\u00e7\u0131klamalar\u0131ndan da anla\u015f\u0131laca\u011f\u0131 gibi yap\u0131m\u0131 en kolay teleskop tipi Newton t\u00fcr\u00fc teleskoptur. Di\u011fer t\u00fcrleri yapan amat\u00f6rler de var ancak bunlar teleskop yap\u0131m\u0131nda uzmanla\u015fm\u0131\u015f ki\u015filerdir ve yap\u0131mlar\u0131 olduk\u00e7a zordur.<\/p>\n\n\n\n Kaynak: http:\/\/atmturk.org\/<\/p>\n\n\n\n <\/p>\n\n\n\n <\/p>\n","protected":false},"excerpt":{"rendered":" Uzaydan gelen her t\u00fcrl\u00fc radyasyonu al\u0131p g\u00f6r\u00fcnt\u00fcleyen astronomlar\u0131n kulland\u0131\u011f\u0131, bir rasathane cihaz\u0131d\u0131r. 1608 y\u0131l\u0131nda Hans Lippershey (Hollandal\u0131 g\u00f6zl\u00fck \u00fcreticisi) taraf\u0131ndan icat edilmi\u015f, 1609 y\u0131l\u0131nda Galileo Galilei taraf\u0131ndan ilk defa, g\u00f6ky\u00fcz\u00fc g\u00f6zlemleri yapmakta kullan\u0131lm\u0131\u015ft\u0131r. Uzaydaki cisimlerden yans\u0131yarak veya do\u011frudan do\u011fruya gelen, g\u00f6zle g\u00f6r\u00fclen \u0131\u015f\u0131k, ultraviyole \u0131\u015f\u0131nlar, k\u0131z\u0131l\u00f6tesi \u0131\u015f\u0131nlar, r\u00f6ntgen \u0131\u015f\u0131nlar\u0131, radyo dalgalar\u0131 gibi her t\u00fcrl\u00fc elektromanyetik…<\/p>\n","protected":false},"author":1,"featured_media":1924,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"_jetpack_memberships_contains_paid_content":false,"footnotes":""},"categories":[42],"tags":[],"class_list":["post-1922","post","type-post","status-publish","format-standard","has-post-thumbnail","hentry","category-teleskop-nedir","wpcat-42-id"],"jetpack_featured_media_url":"https:\/\/i0.wp.com\/www.ikizler.org\/wp-content\/uploads\/2021\/06\/002.png?fit=564%2C528","jetpack_sharing_enabled":true,"_links":{"self":[{"href":"http:\/\/www.ikizler.org\/index.php\/wp-json\/wp\/v2\/posts\/1922","targetHints":{"allow":["GET"]}}],"collection":[{"href":"http:\/\/www.ikizler.org\/index.php\/wp-json\/wp\/v2\/posts"}],"about":[{"href":"http:\/\/www.ikizler.org\/index.php\/wp-json\/wp\/v2\/types\/post"}],"author":[{"embeddable":true,"href":"http:\/\/www.ikizler.org\/index.php\/wp-json\/wp\/v2\/users\/1"}],"replies":[{"embeddable":true,"href":"http:\/\/www.ikizler.org\/index.php\/wp-json\/wp\/v2\/comments?post=1922"}],"version-history":[{"count":5,"href":"http:\/\/www.ikizler.org\/index.php\/wp-json\/wp\/v2\/posts\/1922\/revisions"}],"predecessor-version":[{"id":1932,"href":"http:\/\/www.ikizler.org\/index.php\/wp-json\/wp\/v2\/posts\/1922\/revisions\/1932"}],"wp:featuredmedia":[{"embeddable":true,"href":"http:\/\/www.ikizler.org\/index.php\/wp-json\/wp\/v2\/media\/1924"}],"wp:attachment":[{"href":"http:\/\/www.ikizler.org\/index.php\/wp-json\/wp\/v2\/media?parent=1922"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"http:\/\/www.ikizler.org\/index.php\/wp-json\/wp\/v2\/categories?post=1922"},{"taxonomy":"post_tag","embeddable":true,"href":"http:\/\/www.ikizler.org\/index.php\/wp-json\/wp\/v2\/tags?post=1922"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}
B\u00fcy\u00fctme G\u00fcc\u00fc = Teleskobun Odak Uzakl\u0131\u011f\u0131 \/ G\u00f6zmerce\u011finin Odak Uzakl\u0131\u011f\u0131\u000b\u00d6rne\u011fin 1000 mm odak uzunlu\u011funa sahip teleskopla birlikte 25 mm’lik g\u00f6z merce\u011fi kullan\u0131yorsan\u0131z (1000\u00f7 25=40) 40x b\u00fcy\u00fctme g\u00fcc\u00fc elde edersiniz. B\u00fcy\u00fctme g\u00fcc\u00fcn\u00fc 2 kat artt\u0131rmak parlakl\u0131\u011f\u0131n 1\/4’e d\u00fc\u015fmesine ve netli\u011fin de yar\u0131 yar\u0131ya azalmas\u0131na sebep olur. Bu form\u00fcl teoride istedi\u011finiz kadar b\u00fcy\u00fcltme yapabilece\u011finizi d\u00fc\u015f\u00fcnd\u00fcrse de, bir teleskopla optimum sonucu alabilece\u011finiz azami b\u00fcy\u00fcltme teleskobun objektif \u00e7ap\u0131n\u0131n mm cinsinden 2 kat\u0131d\u0131r. \u00d6rne\u011fimizdeki 90mm’l\u0131k teleskobun sa\u011flayabilece\u011fi azami b\u00fcy\u00fcltme 90 x 2 = 180 kezdir.<\/p>\n\n\n\n![\"\"](\"https:\/\/i0.wp.com\/www.ikizler.org\/wp-content\/uploads\/2021\/06\/001.png?resize=412%2C217\")
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