{"id":47425,"date":"2018-09-01T10:48:05","date_gmt":"2018-09-01T08:48:05","guid":{"rendered":"https:\/\/osr.org\/?p=47425\/"},"modified":"2018-09-01T10:48:05","modified_gmt":"2018-09-01T08:48:05","slug":"nebulalar-ve-dunyamiz","status":"publish","type":"post","link":"https:\/\/osr.org\/tr\/blog\/astronomi\/nebulalar-ve-dunyamiz\/","title":{"rendered":"Nebulalar ve d\u00fcnyam\u0131z"},"content":{"rendered":"

Carina Nebula<\/span><\/h2>\n

Karina Bulutsusu (ayr\u0131ca Karina’daki B\u00fcy\u00fck Bulutsu, Eta Carinae Bulutsusu, veya NGC 3372 olarak da denmektedir), \u00e7evresinde bulunan a\u00e7\u0131k y\u0131ld\u0131z k\u00fcmesi ile birlikte b\u00fcy\u00fck ve parlak bir bulutsudur. Eta Carina ve HD ve HD 93129A, Samanyolu i\u00e7indeki en b\u00fcy\u00fck k\u00fctleli ve parlak y\u0131ld\u0131zlard\u0131r. Bulutsu, Karina tak\u0131my\u0131ld\u0131z\u0131 y\u00f6n\u00fcnde D\u00fcnya’dan yakla\u015f\u0131k olarak 6.500 il\u00e2 10.000 \u0131\u015f\u0131k y\u0131l\u0131 uzakl\u0131kta bulunmaktad\u0131r ve \u00e7oklu O-tipi y\u0131ld\u0131zlar i\u00e7erir.
\nBulutsu, g\u00f6ky\u00fcz\u00fcndeki en b\u00fcy\u00fck salma bulutsudur. Her ne kadar me\u015fhur Orion Bulutsusu’ndan d\u00f6rt kat daha b\u00fcy\u00fck ve parlak olsa da, G\u00fcney yar\u0131k\u00fcrede yer ald\u0131\u011f\u0131ndan daha az bilinen bir bulutsudur. Nicolas Louis de Lacaille taraf\u0131ndan 1751\u201352 y\u0131llar\u0131nda ke\u015ffedilmi\u015ftir.<\/p>\n

B\u00fcy\u00fck parlak bulutsunun k\u00fc\u00e7\u00fck bir \u00f6zelli\u011fi de Eta Carinae’nin \u00e7evresindedir. Bu k\u00fc\u00e7\u00fck bulutsu, Homunculus Bulutsusudur ve 1841 y\u0131l\u0131nda g\u00f6ky\u00fcz\u00fcnde g\u00f6r\u00fclen ikinci parlak y\u0131ld\u0131z olacak kadar b\u00fcy\u00fck patlamayla Eta Carinae taraf\u0131ndan ortaya \u00e7\u0131kar\u0131lm\u0131\u015ft\u0131r.<\/p>\n

Carina Nebula\u2019n\u0131n i\u00e7inde neler var?<\/span><\/h2>\n

Eta Carinae, ayd\u0131nlatma g\u00fcc\u00fc \u00e7ok y\u00fcksek \u00fcst\u00fcn dev bir y\u0131ld\u0131zd\u0131r. K\u00fctlesi, G\u00fcne\u015f k\u00fctlesinden 100 – 150 kat fazla ve ayd\u0131nlatma g\u00fcc\u00fc d\u00f6rt milyon kat daha y\u00fcksektir.
\nBu cisim \u015fu ana kadar b\u00fcy\u00fck bir ayr\u0131nt\u0131yla incelenmi\u015f en b\u00fcy\u00fck y\u0131ld\u0131zd\u0131r. Daha ayd\u0131nl\u0131k ve daha b\u00fcy\u00fck k\u00fctleli y\u0131ld\u0131zlar da vard\u0131r, ancak bu y\u0131ld\u0131zlarda elde edilen veriler bu kadar g\u00fcvenilir de\u011fildir. Bu tip y\u0131ld\u0131zlar\u0131n k\u00fctleleri genellikle G\u00fcne\u015f’ten 80 kat daha fazla ve ayd\u0131nlatma g\u00fcc\u00fc de bir milyon kat daha fazla olabilir. Bu y\u0131ld\u0131zlar \u00e7ok nadirdir ve Eddington s\u0131n\u0131r\u0131 yak\u0131nlar\u0131nda adeta felaketle fl\u00f6rt ederler, radyasyonun d\u0131\u015f bas\u0131nc\u0131 neredeyse yer\u00e7ekimine kar\u015f\u0131 gelecek kadar g\u00fc\u00e7l\u00fcd\u00fcr. G\u00fcne\u015f k\u00fctlesini 120 kat a\u015fan y\u0131ld\u0131zlar teorik olarak Eddington s\u0131n\u0131r\u0131n\u0131 a\u015farlar ve k\u00fctle\u00e7ekim kuvvetleri radyasyon ve gaz\u0131 tutacak kadar g\u00fc\u00e7l\u00fcd\u00fcr. Bunun sonucu olarak yak\u0131n geleceklerinde bir s\u00fcpernova veya \u00fcst\u00fcn nova olabilirler.
\nEta Carinae’n\u0131n etkileri bulutsu \u00fczerinde do\u011frudan g\u00f6r\u00fclebilir. Yukar\u0131daki resimde de g\u00f6r\u00fclen karanl\u0131k damlac\u0131klar ve di\u011fer az g\u00f6r\u00fcnen cisimlerin, uzaktaki b\u00fcy\u00fck k\u00fctleli bir y\u0131ld\u0131z\u0131 i\u015faret eden kuyruklar\u0131 bulunur.<\/p>\n

19. y\u00fczy\u0131lda John Herschel’in Anahtar Deli\u011fi Bulutsusu ad\u0131n\u0131 verdi\u011fi bulutsu, Karina Bulutsusu’nun bir par\u00e7as\u0131d\u0131r. Anahtar Deli\u011fi Bulutsusu, ger\u00e7ekte so\u011fuk molek\u00fcller ve tozun \u00e7ok k\u00fc\u00e7\u00fck ve karanl\u0131k bulutlardaki s\u0131cak parlak lifler ve floresan \u00f6zellikteki gaz ile \u00e7ok daha parlak arka plandaki bulutsuya kar\u015f\u0131 bir siluet olarak kendini g\u00f6sterir.<\/p>\n

Di\u011fer Nebulalar<\/span><\/h2>\n

Nebula ya da bulutsu uzayda bulunan ve geni\u015f alanlara yay\u0131lm\u0131\u015f olan gazlar, toz, Hidrojen, helyum ve di\u011fer iyonize gazlardan olu\u015fan bulutsu yap\u0131. Eskiden galaksileri de kapsayacak \u015fekilde yayg\u0131n g\u00f6k cisimlerine verilen isim iken, astronominin ilerlemesi ile galaksi ile nebula farkl\u0131 anlamlarda kullan\u0131l\u0131r olmaya ba\u015flam\u0131\u015flard\u0131r. Y\u0131ld\u0131zlar aras\u0131nda bulunan bo\u015fluklarda yer alan ve y\u0131ld\u0131zlar\u0131n yayd\u0131klar\u0131 \u0131\u015f\u0131k enerjisi ile g\u00f6r\u00fcn\u00fcr hale gelen yo\u011fun gaz ve toz bulutlar\u0131, galaksilerin temel bile\u015fenlerindendir.<\/p>\n

Bir Nebula olu\u015fmadan \u00f6nce bir y\u0131ld\u0131zd\u0131r. Bu y\u0131ld\u0131z b\u00fcy\u00fcd\u00fckten sonra ya beyaz c\u00fcce ya n\u00f6tron y\u0131ld\u0131z\u0131 ya da bir karadelik olur. Fakat b\u00fct\u00fcn y\u0131ld\u0131zlar bunlardan biri olmadan \u00f6nce k\u0131rm\u0131z\u0131 s\u00fcperdev haline gelir. Bu y\u0131ld\u0131zlar \u00e7ok b\u00fcy\u00fck olduklar\u0131 i\u00e7in i\u00e7ten gelen bas\u0131n\u00e7 ve y\u00fcksek (100.000.000 \u00b0C) s\u0131cakl\u0131\u011f\u0131n etkisiyle uzay bo\u015flu\u011funa gaz salarlar.
\nBu gaz p\u00fcsk\u00fcrmeleri olduk\u00e7a b\u00fcy\u00fck ve h\u0131zl\u0131d\u0131r. Daha sonralar\u0131 bu gazlar yak\u0131nla\u015farak bir gaz bulutu olu\u015ftururlar. Bu gaz bulutunun s\u0131cakl\u0131\u011f\u0131 15.000 \u00b0C den fazlad\u0131r. Bu s\u0131cakl\u0131k ve \u00e7e\u015fitli bas\u0131n\u00e7lar oradaki gazlar (Hidrojen) ile birle\u015ferek f\u00fczyon reaksiyonu ba\u015flat\u0131rlar. Bu f\u00fczyon reaksiyonu yeni bir y\u0131ld\u0131z\u0131n ilk temelleridir. Daha sonra o minik y\u0131ld\u0131zlar b\u00fcy\u00fcr ve anakol y\u0131ld\u0131z\u0131na d\u00f6n\u00fc\u015ft\u00fc\u011f\u00fc zaman ana y\u0131ld\u0131z kadar olmasa da gaz p\u00fcsk\u00fcrtmesi yaparlar. Bu arada ana y\u0131ld\u0131z kahverengi veya beyaz c\u00fcce olup \u00f6mr\u00fcn\u00fc demir ve karbon y\u0131\u011f\u0131n\u0131 olarak tamamlam\u0131\u015ft\u0131r.
\n\u00c7ok parlak y\u0131ld\u0131zlar\u0131 g\u00f6rmek<\/p>\n

G\u00f6ky\u00fcz\u00fcne birer g\u00fcn arayla bak\u0131ld\u0131\u011f\u0131nda \u00f6nceden g\u00f6r\u00fclmeyen \u00e7ok parlak bir y\u0131ld\u0131z g\u00f6r\u00fclebilir. Bunun nedeni bir s\u00fcpernova patlamas\u0131n\u0131n olmas\u0131d\u0131r. S\u00fcpernova patlamalar\u0131 izlemeye de\u011fer olaylard\u0131r. En son kaydedilen patlama 1987 y\u0131l\u0131nda olmu\u015f ve kay\u0131tlara 1987A olarak ge\u00e7mi\u015ftir. *Eski \u00c7a\u011f* d\u00f6nemlerinde \u00c7in’de de izlenmi\u015f bir s\u00fcpernova patlamas\u0131 vard\u0131r. S\u00fcpernova patlamalar\u0131nda k\u0131rm\u0131z\u0131 s\u00fcper devler patlay\u0131p n\u00f6tron y\u0131ld\u0131z\u0131 olu\u015ftururlar. Bazen karadelik olu\u015fur. Karadelik olu\u015fma ihtimali binde birdir. Karadelik olu\u015ftu\u011fu zaman \u00e7evresindeki her \u015feyi \u00e7eker. N\u00f6tron y\u0131ld\u0131z\u0131 olu\u015ftu\u011fu zaman \u00e7evresindekileri karadelik gibi \u00e7ekmez. N\u00f6tron y\u0131ld\u0131z\u0131n\u0131n madde yo\u011funlu\u011fu \u00e7ok fazlad\u0131r.<\/p>\n

Bazen y\u0131ld\u0131zlar s\u00fcpernova ge\u00e7irerek patlarlar. Bunun sonucunda \u00e7evrelerine yava\u015f yava\u015f gaz salmak yerine bir anda salm\u0131\u015f olurlar. Bu arada bu gazlar \u00e7e\u015fitlidir ve reaksiyona girerek \u00e7e\u015fitlili\u011fi artt\u0131r\u0131rlar. Bu da \u00e7ok renkli bir g\u00f6r\u00fcnt\u00fc olu\u015fturur. Bu bulutsular s\u00fcpernova sonucu olu\u015fmu\u015f bulutsular diye adland\u0131r\u0131l\u0131r.
\nS\u00fcpernova sonucu olu\u015fmu\u015flarda gazlar \u00e7e\u015fitli etkiler sayesinde da\u011f\u0131l\u0131rlar ve garip \u015fekiller olu\u015fur. Fakat gezegenimsi bulutsularda gazlar da\u011f\u0131lmad\u0131\u011f\u0131 i\u00e7in simetrikdir. Bir nebulan\u0131n gezegenimsi mi yoksa s\u00fcpernova sonucumu olu\u015ftu\u011fu buna bakarak anla\u015f\u0131labilir.<\/p>\n

Cat eye nebula (Kedi g\u00f6z\u00fc nebulas\u0131)<\/span><\/h2>\n

Yar\u0131m \u0131\u015f\u0131k y\u0131l\u0131 uzunlu\u011fundan biraz daha geni\u015ftir. Kedi g\u00f6z\u00fcn\u00fc and\u0131rmas\u0131 nedeniyle bu isim konmu\u015ftur. D\u00fcnyam\u0131zdan 3000 \u0131\u015f\u0131k y\u0131l\u0131 uzakl\u0131ktad\u0131r. Bu haliyle bir\u00e7ok \u00f6nemli bulu\u015fa da sahiplik yapm\u0131\u015ft\u0131r. <\/p>\n

Orion nebulas\u0131 (Avc\u0131)<\/span><\/h2>\n

Belki de her zaman en \u00e7ok bilinen nebulalar i\u00e7inde olacakt\u0131r. D\u00fcnyadan d\u00fcrb\u00fcnle uygun bir yerdeyseniz g\u00f6zlemleyebilirsiniz. Bu nebulan\u0131n \u0131\u015f\u0131\u011f\u0131, i\u00e7 b\u00f6lgesinde yeni do\u011fmakta olan g\u00fc\u00e7l\u00fc \u0131\u015f\u0131ldayan y\u0131ld\u0131zlar\u0131n ayd\u0131nlat\u0131lmas\u0131ndan kaynaklan\u0131r. Bulut ilk kez 1610’da Nicolas-Claude Fabri de Peiresc taraf\u0131ndan belgelendirmi\u015ftir. Avc\u0131n\u0131n belirgin \u015fekli d\u00f6rt belirgin y\u0131ld\u0131zdan olu\u015fan boyu eninin iki kat\u0131 kadar olan bir dikd\u00f6rtgen ve bu dikd\u00f6rtgenin merkezinde \u00e7apraz durmakta olan \u00fc\u00e7 ayr\u0131 y\u0131ld\u0131zd\u0131r. Betelgeuse avc\u0131n\u0131n sa\u011f omzuna, Bellatrix sol omzuna, Rigel sol aya\u011f\u0131na ve Saif de sa\u011f aya\u011f\u0131na denk gelir. Ortadaki \u00fc\u00e7 \u00e7apraz y\u0131ld\u0131z (alttan \u00fcste s\u0131rayla Alnitak, Alnilam ve Mintaka) avc\u0131n\u0131n kemerini (Orion ku\u015fa\u011f\u0131 olarak da bilinir) olu\u015fturur. Ku\u015fa\u011f\u0131n alt\u0131nda bulunan Orion Bulutsusu (nebulas\u0131) avc\u0131n\u0131n k\u0131l\u0131c\u0131d\u0131r. Heka ad\u0131ndaki avc\u0131n\u0131n ba\u015f\u0131n\u0131 simgleyen k\u0131s\u0131m asl\u0131nda \u00fc\u00e7 daha s\u00f6n\u00fck y\u0131ld\u0131zdan meydana gelir. Betelgeuse’un \u00fcst\u00fcndeki y\u0131ld\u0131zlar avc\u0131n\u0131n sa\u011f kolunu Bellatrix’den \u00f6tede olan y\u0131ld\u0131zlarda avc\u0131n\u0131n kalkan\u0131n\u0131 olu\u015fturur.<\/p>\n

Butterfly nebula (Kelebek Bulutsusu)<\/span><\/h2>\n

Bu bulutsu, Akrep tak\u0131my\u0131ld\u0131z\u0131 y\u00f6n\u00fcnde yakla\u015f\u0131k olarak 4.000 \u0131\u015f\u0131k y\u0131l\u0131 uzakl\u0131kta bulunan \u00e7iftkutuplu bir gezegenimsi bulutsudur. Bu, g\u00f6zlenmi\u015f en ilgin\u00e7 ve karma\u015f\u0131k gezegenimsi bulutsulardan biri olarak bilinir. Bu harika bulutsuyu olu\u015fturan y\u0131ld\u0131z\u0131n \u00e7ok b\u00fcy\u00fck bir y\u0131ld\u0131z oldu\u011fu bilinir ve bu nedenle de gizemini korur. Kelebek bulutsusunun ana y\u0131ld\u0131z\u0131 hen\u00fcz hi\u00e7 g\u00f6zlenememi\u015ftir. Bu merkezi y\u0131ld\u0131z, ekvatoryal disk gaz ve toz bulutuyla \u00e7evrelenmi\u015ftir. Bulutsu, 1880 y\u0131l\u0131nda Edward Barnard taraf\u0131ndan ke\u015ffedilmi\u015ftir.<\/p>\n

Crap nebula (Yenge\u00e7 Bulutsusu)<\/span><\/h2>\n

Yenge\u00e7 Bulutsusu Bo\u011fa tak\u0131my\u0131ld\u0131z\u0131 y\u00f6n\u00fcnde yer alan bir s\u00fcpernova kal\u0131nt\u0131s\u0131 olarak bilinir. Bulutsu ilk olarak 1731 y\u0131l\u0131nda John Bevis taraf\u0131ndan g\u00f6zlemlenmi\u015ftir. Bulutsu, D\u00fcnya’dan 4 Temmuz 1054 tarihinde g\u00f6r\u00fclen bir s\u00fcpernova patlamas\u0131n\u0131n geriye kalan k\u0131r\u0131nt\u0131lard\u0131r. Bu tarih biliniyor; \u00e7\u00fcnk\u00fc \u00c7inli g\u00f6kbilimciler bir y\u0131ld\u0131z\u0131n aniden g\u00fcnd\u00fcz bile g\u00f6r\u00fclebilecek kadar parlad\u0131\u011f\u0131n\u0131 kay\u0131tlara ge\u00e7mi\u015fler. Bu y\u0131ld\u0131z parlakl\u0131\u011f\u0131 sayesinde, 23 g\u00fcn s\u00fcresince g\u00fcnd\u00fcz g\u00f6zlenmi\u015f. Bulutsu, yengece benzedi\u011fi i\u00e7in bu ad\u0131 alm\u0131\u015ft\u0131r. D\u00fcnyadan yakla\u015f\u0131k 7000 \u0131\u015f\u0131k y\u0131l\u0131 uzakta bulunan bulutsunun \u00e7ap\u0131 11 \u0131\u015f\u0131k y\u0131l\u0131d\u0131r ve saniyede 1.800 km h\u0131zla geni\u015flemektedir. K\u0131sacas\u0131, s\u00fcrekli geni\u015fliyor. <\/p>\n

1968 y\u0131l\u0131nda, bulutsunun merkezinde patlayan y\u0131ld\u0131zdan kalan, saniyede otuz kez d\u00f6nen ve gama \u0131\u015f\u0131nlar\u0131ndan radyo dalgalar\u0131na kadar \u0131\u015f\u0131n\u0131m at\u0131mlar\u0131 yayan Yenge\u00e7 atarcas\u0131 ke\u015ffedildi. Bulutsu, tarihi bir s\u00fcpernova patlamas\u0131 sayesinde tan\u0131mlanan ilk g\u00f6kcismi olarak tarihe ge\u00e7ti.<\/p>\n

Bu bulutsu kendisini \u00f6rten g\u00f6k cisimlerini incelemek i\u00e7in bir \u0131\u015f\u0131n\u0131m kayna\u011f\u0131 olarak davran\u0131r. 1950 ve 1960’larda G\u00fcne\u015f’in tac\u0131, i\u00e7inden ge\u00e7en Yenge\u00e7 Bulutsusu’nun radyo dalgalar\u0131 sayesinde haritaland\u0131r\u0131lm\u0131\u015ft\u0131. Son zamanlarda da Sat\u00fcrn’\u00fcn uydusu Titan’\u0131n gazyuvar\u0131n\u0131n kal\u0131nl\u0131\u011f\u0131, gazyuvar\u0131n bulutsudan gelen X \u0131\u015f\u0131nlar\u0131n\u0131 engellemesi sayesinde \u00f6l\u00e7\u00fclebilmi\u015ftir.<\/p>\n

The eagle nebula (Kartal Bulutsusu)<\/span><\/h2>\n

Y\u0131lan tak\u0131my\u0131ld\u0131z\u0131nda bulunan gen\u00e7 bir a\u00e7\u0131k y\u0131ld\u0131z k\u00fcmesidir. Ad\u0131 kartal\u0131 an\u0131msatan \u015feklinden kaynaklanmaktad\u0131r. Bu bulutsunun merkezi yak\u0131n\u0131nda y\u00fckselen ve fil hortumlar\u0131 veya Yarat\u0131l\u0131\u015f S\u00fctunlar\u0131 olarak tan\u0131mlanan yo\u011fun, tozlu s\u00fctunlar \u0131\u015f\u0131ky\u0131llar\u0131 uzunlu\u011fundad\u0131r; ancak y\u0131ld\u0131zlar\u0131 olu\u015fturmak \u00fczere k\u00fctle\u00e7ekimsel olarak b\u00fcz\u00fclmektedir. K\u00fcme y\u0131ld\u0131zlar\u0131ndan gelen enerji y\u00fckl\u00fc \u0131\u015f\u0131n\u0131mlar, s\u00fctunlar\u0131n u\u00e7lar\u0131 yak\u0131n\u0131nda bulunan malzemeyi a\u015f\u0131nd\u0131rarak, \u00f6n\u00fcnde sonunda i\u00e7lerinde g\u00f6m\u00fcl\u00fc durumdayken olu\u015fan yeni y\u0131ld\u0131zlar\u0131 ortaya \u00e7\u0131karmaktad\u0131r. Bulutsunun sol \u00fcst kenar\u0131ndan uzanan bir di\u011fer tozlu y\u0131ld\u0131z olu\u015fum s\u00fctunu ise Kartal Bulutsusu’nun Perisi olarak tan\u0131nmaktad\u0131r. Bulutsudaki en parlak y\u0131ld\u0131z 8,24 g\u00f6r\u00fcn\u00fcr parlakl\u0131\u011f\u0131yla iyi bir d\u00fcrb\u00fcnle kolayca g\u00f6zlenebilir.<\/p>\n

Pillars of creation (yarat\u0131\u015f\u0131l s\u00fctunlar\u0131)<\/span><\/h2>\n

\u0130smini yarat\u0131l\u0131\u015f s\u00fctunu olmas\u0131n\u0131n sebebi bir \u00e7ok y\u0131ld\u0131z do\u011fuyor olmas\u0131d\u0131r. Adeta bir y\u0131ld\u0131z fabrikas\u0131 g\u00f6revi g\u00f6ren bu nebula bir \u00e7ok y\u0131ld\u0131z bar\u0131nd\u0131rmaktad\u0131r. Di\u011fer yandan burada bir\u00e7ok y\u0131ld\u0131z da kayboluyor. K\u0131sacas\u0131 buras\u0131 do\u011fu\u015fun ve yok olu\u015fun yeri olarak da biliniyor. Hepimizin g\u00f6z\u00fcn\u00fcn \u00f6n\u00fcnde bir\u00e7ok gen\u00e7 y\u0131ld\u0131z meydana geliyor ve hemen de yok olabiliyorlar. Bu g\u00fczel bulutsuyu Hubble yeniden g\u00f6r\u00fcnt\u00fcledi ve bu sefer eskisine g\u00f6re \u00e7ok daha net bir foto\u011fraf \u00e7ekmeyi ba\u015fard\u0131. Andromeda Galaksisi’nde \u00e7ekilen 13 bin yeni foto\u011fraf\u0131n bir araya getirilmesiyle, teleskop \u015fimdiye kadar ki en b\u00fcy\u00fck foto\u011fraf\u0131 olu\u015fturdu.
\nG\u00f6r\u00fcnt\u00fcler Amerika Birle\u015fik Devletleri’nin \u015fehrinde Amerikan Astronomi Toplulu\u011fu’nun d\u00fczenledi\u011fi toplant\u0131da payla\u015f\u0131ld\u0131.
\nToplant\u0131da, Arizona Devlet \u00dcniversitesi’nden Dr. Paul Scowen, bu g\u00f6r\u00fcnt\u00fcleri “Eski bir dostun yeni resimleri” olarak adland\u0131rd\u0131.<\/p>\n

Hilal bulutsusu<\/span><\/h2>\n

Hil\u00e2l Bulutsusu, Ku\u011fu tak\u0131my\u0131ld\u0131z\u0131 y\u00f6n\u00fcnde ve yakla\u015f\u0131k 5000 \u0131\u015f\u0131k y\u0131l\u0131 uzakl\u0131kta bulunan bir salma bulutsusu. Wilhelm Herschel taraf\u0131ndan 15 Aral\u0131k 1792 tarihinde ke\u015ffedilmi\u015ftir.
\nNGC 6888’in merkezindeki y\u0131ld\u0131z bir Wolf-Rayet y\u0131ld\u0131z\u0131 olarak s\u0131n\u0131fland\u0131r\u0131lm\u0131\u015ft\u0131r WR 136 (HD 192163). Y\u0131ld\u0131z her 10.000 y\u0131lda G\u00fcne\u015f k\u00fctlesine e\u015fit miktarda olmak \u00fczere, d\u0131\u015f kabu\u011funu g\u00fc\u00e7l\u00fc bir y\u0131ld\u0131z r\u00fczgar\u0131yla f\u0131rlat\u0131p atmaktad\u0131r. Bulutsunun karma\u015f\u0131k yap\u0131s\u0131, b\u00fcy\u00fck bir olas\u0131l\u0131kla bu g\u00fc\u00e7l\u00fc r\u00fczgar\u0131n daha erken bir evrede f\u0131rlat\u0131l\u0131p at\u0131lan bir malzeme ile etkile\u015fime girmesinin sonucudur. Yak\u0131t\u0131n\u0131 muazzam bir h\u0131zla t\u00fcketen ve \u00f6mr\u00fcn\u00fcn sonlar\u0131na yakla\u015fan bu y\u0131ld\u0131z, en sonunda g\u00f6r\u00fclmeye de\u011fer bir s\u00fcpernova patlamas\u0131yla parlay\u0131p, s\u00f6n\u00fcp gidecektir.
\nHilal Bulutsusu yakla\u015f\u0131k 25 \u0131\u015f\u0131k y\u0131l\u0131 \u00e7ap\u0131nda, merkezindeki parlak ve b\u00fcy\u00fck k\u00fctleli y\u0131ld\u0131zdan gelen r\u00fczgarla \u015fi\u015firilmi\u015f evrensel bir kabarc\u0131kt\u0131r. Yukar\u0131daki keskin teleskop g\u00f6r\u00fcnt\u00fcs\u00fcnde, bu r\u00fczgar\u0131n \u015fi\u015firdi\u011fi bulutsu i\u00e7erisindeki hidrojen ve oksijen atomlar\u0131ndan gelen \u0131\u015f\u0131\u011f\u0131 ay\u0131rt eden dar bant s\u00fczge\u00e7 verileri kullan\u0131lm\u0131\u015ft\u0131r. G\u00f6r\u00fcnt\u00fcdeki ayr\u0131nt\u0131l\u0131 k\u0131vr\u0131m ve iplik\u00e7ikleri sarmalam\u0131\u015f gibi g\u00f6r\u00fcnen mavi ye\u015fil renk, oksijen atomlar\u0131 taraf\u0131ndan \u00fcretilmektedir. Bulutsu ile birlikte g\u00f6r\u00fclen merkezindeki y\u0131ld\u0131z bir Wolf-Rayet y\u0131ld\u0131z\u0131 olarak s\u0131n\u0131fland\u0131r\u0131lm\u0131\u015ft\u0131r . Y\u0131ld\u0131z her 10.000 y\u0131lda G\u00fcne\u015f k\u00fctlesine e\u015fit miktarda olmak \u00fczere, d\u0131\u015f kabu\u011funu g\u00fc\u00e7l\u00fc bir y\u0131ld\u0131z r\u00fczgar\u0131yla f\u0131rlat\u0131p atmaktad\u0131r. Bulutsunun karma\u015f\u0131k yap\u0131s\u0131, b\u00fcy\u00fck bir olas\u0131l\u0131kla bu g\u00fc\u00e7l\u00fc r\u00fczgar\u0131n daha erken bir evrede f\u0131rlat\u0131l\u0131p at\u0131lan bir malzeme ile etkile\u015fime girmesinin sonucudur.<\/p>\n","protected":false},"excerpt":{"rendered":"

Carina Nebula Karina Bulutsusu (ayr\u0131ca Karina’daki B\u00fcy\u00fck Bulutsu, Eta Carinae Bulutsusu, veya NGC 3372 olarak da denmektedir), \u00e7evresinde bulunan a\u00e7\u0131k y\u0131ld\u0131z k\u00fcmesi ile birlikte b\u00fcy\u00fck ve parlak bir bulutsudur. Eta Carina ve HD ve HD 93129A, Samanyolu i\u00e7indeki en b\u00fcy\u00fck k\u00fctleli ve parlak y\u0131ld\u0131zlard\u0131r. Bulutsu, Karina tak\u0131my\u0131ld\u0131z\u0131 y\u00f6n\u00fcnde D\u00fcnya’dan yakla\u015f\u0131k olarak 6.500 il\u00e2 10.000 \u0131\u015f\u0131k […]<\/p>\n","protected":false},"author":23,"featured_media":0,"comment_status":"closed","ping_status":"closed","sticky":false,"template":"","format":"standard","meta":{"_acf_changed":false,"inline_featured_image":false,"footnotes":""},"categories":[506],"tags":[],"class_list":["post-47425","post","type-post","status-publish","format-standard","hentry","category-astronomi"],"acf":[],"yoast_head":"\nNebulalar ve d\u00fcnyam\u0131z - Online Star Register<\/title>\n<meta name=\"robots\" content=\"index, follow, max-snippet:-1, max-image-preview:large, max-video-preview:-1\" \/>\n<link rel=\"canonical\" href=\"https:\/\/osr.org\/tr\/blog\/astronomi\/nebulalar-ve-dunyamiz\/\" \/>\n<meta property=\"og:locale\" content=\"tr_TR\" \/>\n<meta property=\"og:type\" content=\"article\" \/>\n<meta property=\"og:title\" content=\"Nebulalar ve d\u00fcnyam\u0131z - Online Star Register\" \/>\n<meta property=\"og:description\" content=\"Carina Nebula Karina Bulutsusu (ayr\u0131ca Karina’daki B\u00fcy\u00fck Bulutsu, Eta Carinae Bulutsusu, veya NGC 3372 olarak da denmektedir), \u00e7evresinde bulunan a\u00e7\u0131k y\u0131ld\u0131z k\u00fcmesi ile birlikte b\u00fcy\u00fck ve parlak bir bulutsudur. Eta Carina ve HD ve HD 93129A, Samanyolu i\u00e7indeki en b\u00fcy\u00fck k\u00fctleli ve parlak y\u0131ld\u0131zlard\u0131r. 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