{"id":62814,"date":"2019-04-06T21:55:46","date_gmt":"2019-04-06T19:55:46","guid":{"rendered":"https:\/\/osr.org\/?p=62814"},"modified":"2019-04-06T21:55:46","modified_gmt":"2019-04-06T19:55:46","slug":"9-degisken-yildiz-kesfettiler","status":"publish","type":"post","link":"https:\/\/osr.org\/tr\/blog\/astronomi\/9-degisken-yildiz-kesfettiler\/","title":{"rendered":"9 De\u011fi\u015fken Y\u0131ld\u0131z Ke\u015ffettiler"},"content":{"rendered":"

Kepler, y\u0131ld\u0131zlar ve tarih\u00e7esi<\/span><\/h2>\n

D\u00fcnyan\u0131n her yerinde yo\u011fun bir \u015fekilde uzay\u0131 ke\u015ffetme \u00e7al\u0131\u015fmalar\u0131 devam ederken, yeni bir ke\u015fif de \u015eili’li astronomlardan geldi. Uzun zamand\u0131r g\u00f6ky\u00fcz\u00fc inceleme \u00e7al\u0131\u015fmalar\u0131 yapan bu grup, 9 adet de\u011fi\u015fken y\u0131ld\u0131z ke\u015ffetti.<\/p>\n

Peki nedir bu de\u011fi\u015fken y\u0131ld\u0131zlar? K\u0131sa ve anla\u015f\u0131l\u0131r bir \u015fekilde ifade etmek gerekirse; de\u011fi\u015fken y\u0131ld\u0131zlar, parlakl\u0131klar\u0131 zaman i\u00e7erisinde de\u011fi\u015fen y\u0131ld\u0131zlard\u0131r. Bu de\u011fi\u015fiklik gen\u00e7 ya\u015flarda ger\u00e7ekle\u015febildi\u011fi gibi, y\u0131ld\u0131zlar \u00e7ok ya\u015fl\u0131 iken de ger\u00e7ekle\u015febilir.<\/p>\n

Bu yeni ke\u015fif, astronomlar i\u00e7in olduk\u00e7a \u00f6nemli \u00e7\u00fcnk\u00fc bilim insanlar\u0131na y\u0131ld\u0131zlar\u0131n yap\u0131sal durumlar\u0131 ve evrimle\u015fme s\u00fcreci hakk\u0131nda ipu\u00e7ular\u0131 verebilir. Ayn\u0131 zamanda, evrendeki uzakl\u0131k kavram\u0131n\u0131 da daha iyi anlamaya yard\u0131mc\u0131 olabilir. Asl\u0131nda astronominin bu dal\u0131, belki de en pop\u00fcler ve en eski bran\u015flar aras\u0131nda yer al\u0131yor. Fakat yeni ke\u015fifler yaparken, uzun vadeli \u00e7al\u0131\u015fmalar ve hatas\u0131z veriler toplanmas\u0131 gerekiyor.<\/p>\n

Bu kadar b\u00fcy\u00fck hacimli verilerin toplanmas\u0131 ve i\u015flenmesi s\u0131ras\u0131nda da zaman zaman sistematik aksakl\u0131klar meydana gelebiliyor. Yeni y\u0131ld\u0131zlar\u0131n ke\u015ffi ile y\u0131ld\u0131zlar aras\u0131 mesafelerin \u00f6l\u00e7\u00fcm\u00fcnde ya\u015fanm\u0131\u015f olabilecek hatalar hakk\u0131nda da fikir edinilmesi umuluyor.<\/p>\n

De\u011fi\u015fen y\u0131ld\u0131zlar<\/span><\/h2>\n

De\u011fi\u015fen Y\u0131ld\u0131z, parlakl\u0131klar\u0131 zaman i\u00e7inde de\u011fi\u015fen y\u0131ld\u0131zlard\u0131r. Parlakl\u0131klar\u0131 genelde ya \u00e7ok gen\u00e7ken, ya da \u00e7ok ya\u015fl\u0131 iken de\u011fi\u015fir. Bunun nedeni, ya geni\u015fleme, daralma, p\u00fcsk\u00fcrme gibi y\u0131ld\u0131z\u0131n i\u00e7 dinami\u011finden; ya da iki ya da daha fazla y\u0131ld\u0131z\u0131n birbirlerinin y\u00f6r\u00fcngelerinde d\u00f6nerken olu\u015fturduklar\u0131 tutulmalardan kaynaklanan d\u0131\u015f dinamiklerden dolay\u0131 olu\u015fur. 2000 y\u0131l\u0131na kadar 30,000’in \u00fczerinde de\u011fi\u015fken y\u0131ld\u0131z bulunup kataloglanm\u0131\u015ft\u0131r. Ayr\u0131ca 14,000 kadar ba\u015fka y\u0131ld\u0131zda parlakl\u0131k de\u011fi\u015fiminden \u015f\u00fcphelenilmektedir. G\u00fcne\u015fimiz ve Kutup Y\u0131ld\u0131z\u0131 dahil olmak \u00fczere bir\u00e7ok y\u0131ld\u0131z\u0131n, yeterli duyarl\u0131l\u0131kta \u00f6l\u00e7\u00fcld\u00fc\u011f\u00fcnde, parlakl\u0131klar\u0131 de\u011fi\u015fmektedir.<\/p>\n

De\u011fi\u015fenlik i\u00e7in en yayg\u0131n t\u00fcr parlakl\u0131k de\u011fi\u015fimidir ama di\u011fer t\u00fcrlerde de tayflarda \u00e7ok \u00f6zel de\u011fi\u015fiklikler meydana gelir. G\u00f6kbilimciler, g\u00f6zlemledikleri tayf de\u011fi\u015fikliklerini \u0131\u015f\u0131k e\u011frisi verileri ile birle\u015ftirerek yeni tan\u0131mlamalar yapm\u0131\u015flard\u0131r.<\/p>\n

De\u011fi\u015fen y\u0131ld\u0131z g\u00f6zlemleri<\/span><\/h2>\n

De\u011fi\u015fen y\u0131ld\u0131z g\u00f6zlemleri, bir ekseninde g\u00f6r\u00fcn\u00fcr parlakl\u0131k (kadir), di\u011ferinde birimi genellikle J\u00fclyen G\u00fcn\u00fc (JG) olan zaman cinsinden \u0131\u015f\u0131k e\u011frisi denen bir grafik \u00fczerine i\u015faretlenir. Y-ekseninde parlakl\u0131k \u00f6l\u00e7e\u011fi a\u015fa\u011f\u0131dan yukar\u0131 do\u011fru artacak \u015fekilde ve X-ekseninde g\u00fcn, soldan sa\u011fa artacak \u015fekilde \u00e7izilir. Y\u0131ld\u0131zlar\u0131n d\u00f6nemsel davran\u0131\u015flar\u0131 hakk\u0131ndaki bilgiler, \u00f6rten \u00e7ift y\u0131ld\u0131zlar\u0131n y\u00f6r\u00fcnge d\u00f6nemleri ve y\u0131ld\u0131z patlamalar\u0131n\u0131n d\u00fczenlilik ya da d\u00fczensizlik derecesi, \u0131\u015f\u0131k e\u011frisinden yararlan\u0131larak bulunabilir. I\u015f\u0131k e\u011frisinin daha ayr\u0131nt\u0131l\u0131 incelenmesi, g\u00f6kbilimcilerin y\u0131ld\u0131zlar\u0131n k\u00fctlelerini ya da boyutlar\u0131n\u0131 hesaplamas\u0131n\u0131 sa\u011flar. Onlarca y\u0131ll\u0131k g\u00f6zlem verileri, bir y\u0131ld\u0131z\u0131n de\u011fi\u015fim d\u00f6nemini a\u00e7\u0131\u011fa \u00e7\u0131kart\u0131r. Hatta bu durum, y\u0131ld\u0131z\u0131n yap\u0131sal de\u011fi\u015fikli\u011finin bir i\u015fareti bile olabilir.<\/p>\n

De\u011fi\u015fen y\u0131ld\u0131zlar\u0131n k\u0131sa zaman \u00f6l\u00e7eklerinde (veya anl\u0131k) olu\u015fan de\u011fi\u015fimlerine ait parametreler, evrimleri boyunca daha uzun zaman \u00f6l\u00e7ekli de\u011fi\u015fimler de g\u00f6sterebilmektedir. \u00d6rne\u011fin bile\u015fenleri aras\u0131nda madde al\u0131\u015fveri\u015fi olan k\u0131sa d\u00f6nemli bir \u00e7ift y\u0131ld\u0131z\u0131n fotometrik ve tayfsal g\u00f6zlemlerinde bu etkinli\u011fe ili\u015fkin izler k\u0131sa zaman \u00f6l\u00e7eklerinde de\u011fi\u015fimler yarat\u0131rken, uzun vadede sistemin y\u00f6r\u00fcnge d\u00f6neminin de\u011fi\u015fim g\u00f6stermesine neden olacakt\u0131r. Delta Scuti (\u03b4 Scuti) t\u00fcr\u00fc zonklayan bir de\u011fi\u015fenin, zonklama d\u00f6neminin s\u00fcresi, y\u0131ld\u0131z evrimle\u015ftik\u00e7e g\u00f6sterece\u011fi \u00e7ap de\u011fi\u015fiminden etkilenecektir. De\u011fi\u015fen y\u0131ld\u0131zlar\u0131n tipik fotometrik parametrelerinin, uzun zaman \u00f6l\u00e7ekleri i\u00e7inde izlenmesi, parlakl\u0131k ve renk de\u011fi\u015fimine neden olan fiziksel s\u00fcre\u00e7lerin daha iyi anla\u015f\u0131lmas\u0131n\u0131 sa\u011flayacakt\u0131r. Ancak eldeki g\u00f6zlemsel veri miktar\u0131, bu anlamda bir irdeleme i\u00e7in hen\u00fcz yeterli boyutlarda de\u011fildir ve g\u00f6zlemlerin b\u00fcy\u00fck bir k\u0131sm\u0131 gelecek ku\u015faklara miras olarak b\u0131rak\u0131lmaktad\u0131r. Bu a\u00e7\u0131dan bak\u0131ld\u0131\u011f\u0131nda de\u011fi\u015fen y\u0131ld\u0131zlar\u0131n uzun zaman aral\u0131\u011f\u0131na da\u011f\u0131lm\u0131\u015f kesintisiz g\u00f6zlemlerinin yap\u0131lmas\u0131 ve bu g\u00f6zlemlerin sistematik olarak ar\u015fivlenmesi b\u00fcy\u00fck \u00f6nem ta\u015f\u0131maktad\u0131r.<\/p>\n

De\u011fi\u015fen y\u0131ld\u0131z \u00e7al\u0131\u015fmalar\u0131<\/span><\/h2>\n

G\u00fcn\u00fcm\u00fczde bir\u00e7ok uluslararas\u0131 hakemli dergiler, de\u011fi\u015fen y\u0131ld\u0131zlar \u00fczerine yap\u0131lm\u0131\u015f \u00e7al\u0131\u015fmalar\u0131 yay\u0131na kabul ederken, fazla yer tuttu\u011fu gerek\u00e7esi ile orijinal g\u00f6zlem verilerini yay\u0131nlamaktan ka\u00e7\u0131nmaktad\u0131r. Bu ise zaman i\u00e7inde eldeki orijinal g\u00f6zlem verisinin bir \u015fekilde kaybolmas\u0131na yol a\u00e7maktad\u0131r. Bunu \u00f6nlemek amac\u0131 ile Uluslararas\u0131 Astronomi Birli\u011fi IAU’nun (International Astronomical Union) komisyonlar\u0131 uzun s\u00fcreden beri de\u011fi\u015fen y\u0131ld\u0131zlar\u0131n yay\u0131nlanmam\u0131\u015f fotometrik g\u00f6zlemlerinin ar\u015fivlenmesini \u00fcstlenmi\u015flerdir. Viyana G\u00f6zlemevi’nden M. Breger’in \u00f6nderli\u011finde ba\u015flayan ve \u015fu anda Nebraska \u00dcniversitesi’nden E. Schmidt ile devam eden bu organizasyon, g\u00f6zlemlerin elektronik formatta CDS (Centre de Donn\u00e9es Astronomiques de Strasbourg) veri taban\u0131 yolu ile ar\u015fivlenmesini ve da\u011f\u0131t\u0131m\u0131n\u0131 ger\u00e7ekle\u015ftirmektedir. Ar\u015fivde yer alan y\u0131ld\u0131zlar\u0131n g\u00f6zlemlerine ili\u015fkin bilgiler d\u00fczenli olarak IBVS (Information Bulletin of Variable Stars, Konkoly Obs., Budapest) periyodi\u011finde yay\u0131nlanmaktad\u0131r. De\u011fi\u015fen y\u0131ld\u0131zlar konusunda genel taramalar yapmak ve bilgi eri\u015fimi sa\u011flamak i\u00e7in \u00e7e\u015fitli kataloglar ve elektronik veri tabanlar\u0131 mevcuttur. <\/p>\n

De\u011fi\u015fen y\u0131ld\u0131z isimleri<\/span><\/h2>\n

De\u011fi\u015fen y\u0131ld\u0131z isimleri, Uluslararas\u0131 Astronomi Birli\u011fi (I.A.U.) taraf\u0131ndan atanan bir komite taraf\u0131ndan belirlenir. Adland\u0131rma, bir tak\u0131my\u0131ld\u0131z i\u00e7indeki de\u011fi\u015fen y\u0131ld\u0131zlar\u0131n ke\u015ffedilme s\u0131ras\u0131na g\u00f6re yap\u0131l\u0131r. Bulunan y\u0131ld\u0131z\u0131n e\u011fer Yunan harfi ile ba\u015flayan ismi varsa, y\u0131ld\u0131z o adla an\u0131lmaya devam eder. Aksi takdirde, bir tak\u0131my\u0131ld\u0131zdaki ilk de\u011fi\u015fen y\u0131ld\u0131z R harfi ile adland\u0131r\u0131l\u0131r, ondan sonraki S olur ve bu \u015fekilde Z’ye kadar devam eder. Bir sonraki y\u0131ld\u0131z RR olarak isimlendirilir, sonra RS’den RZ’ye kadar; SS’den SZ’ye kadar adland\u0131rma devam eder ve b\u00f6ylece ZZ’ye gelinir. Bundan sonra alfabede ba\u015fa d\u00f6n\u00fcl\u00fcr, ve AA, AB ile ba\u015flay\u0131p QZ’ye kadar devam eder. J harfinin kullan\u0131lmad\u0131\u011f\u0131 bu sistem 334 ismi kapsar. Samanyolu’ndaki baz\u0131 tak\u0131my\u0131ld\u0131zlarda o kadar \u00e7ok de\u011fi\u015fen y\u0131ld\u0131z vard\u0131r ki, bunlar i\u00e7in ek terimler gerekmektedir. QZ’den sonraki de\u011fi\u015fenler V335, V336 vb. olarak adland\u0131r\u0131l\u0131rlar. Sonra y\u0131ld\u0131zlar\u0131 simgeleyen harfler tak\u0131my\u0131ld\u0131z\u0131n latince ad\u0131n\u0131n \u2013in hali ile birle\u015ftirilir. En yayg\u0131n olarak, AAVSO’ya yollanacak raporlarda zorunlu oldu\u011fu gibi, \u00fc\u00e7 harflik k\u0131saltma kullan\u0131l\u0131r.<\/p>\n

Bu terminolojik sistem ilk defa 1800’lerin ortalar\u0131nda Friedrich Argelander taraf\u0131ndan ortaya at\u0131lm\u0131\u015ft\u0131r. Argelander’in bu s\u0131ralamaya b\u00fcy\u00fck R ile ba\u015flamas\u0131n\u0131n iki nedeni vard\u0131: K\u00fc\u00e7\u00fck harfler ve alfabenin ilk s\u0131ras\u0131ndaki harfler di\u011fer cisimlere ayr\u0131lm\u0131\u015f; b\u00fcy\u00fck harfler ve alfabenin sonlar\u0131ndaki harfler kullan\u0131lmam\u0131\u015ft\u0131. Ayr\u0131ca Argelander y\u0131ld\u0131z de\u011fi\u015fkenli\u011finin nadir bir olay oldu\u011funu ve bir tak\u0131my\u0131ld\u0131z i\u00e7inde 9’dan fazla de\u011fi\u015fen y\u0131ld\u0131z\u0131n yer alamayaca\u011f\u0131n\u0131 d\u00fc\u015f\u00fcn\u00fcyordu (bug\u00fcn bunun kesinlikle do\u011fru olmad\u0131\u011f\u0131n\u0131 biliyoruz).<\/p>\n

De\u011fi\u015fen y\u0131ld\u0131z b\u00fcnyeleri<\/span><\/h2>\n

Zonklayan de\u011fi\u015fenler, y\u00fczey katmanlar\u0131nda d\u00f6nemsel geni\u015fleme g\u00f6steren y\u0131ld\u0131zlard\u0131r. Zonklamalar, radyal (merkezden yay\u0131lan) ya da radyal olmayan \u015fekildedir. Radyal at\u0131ml\u0131 bir y\u0131ld\u0131z\u0131n bi\u00e7imi k\u00fcresel kal\u0131r, oysaki radyal olmayan at\u0131mlar yapan bir y\u0131ld\u0131z, d\u00f6nemsel olarak k\u00fcresellikten sapabilir. A\u015fa\u011f\u0131daki zonklayan de\u011fi\u015fken y\u0131ld\u0131z tipleri, at\u0131m d\u00f6nemleri, k\u00fctleleri ve y\u0131ld\u0131z etraf\u0131ndaki evrimsel durumlar\u0131 ile at\u0131m karakterleri bak\u0131m\u0131ndan birbirlerinden ayr\u0131labilir.<\/p>\n

Parlakl\u0131klar\u0131ndaki de\u011fi\u015fim 0,1 ila 2 kadir fark\u0131 aras\u0131nda olur. Bu de\u011fi\u015fim \u00f6nce ani bir art\u0131\u015f, sonra yava\u015f bir azalma olarak g\u00f6r\u00fcl\u00fcr. Sefelerin uzakl\u0131klar\u0131yla, mutlak parlakl\u0131klar\u0131 (belirli bir uzakl\u0131ktan (10 parsek), \u00f6l\u00e7\u00fclen parlakl\u0131k) aras\u0131nda bir ili\u015fki vard\u0131r. Bu nedenle g\u00f6kadalar\u0131n ya da k\u00fcresel k\u00fcmelerin uzakl\u0131klar\u0131 \u00f6l\u00e7\u00fcl\u00fcrken, i\u00e7lerinde bulunan bu y\u0131ld\u0131zlardan yararlan\u0131l\u0131r.<\/p>\n

Beta Cephei (\u03b2 Cephei) de\u011fi\u015fenleri, k\u0131sa d\u00f6nemli \u0131\u015f\u0131k ve dikine h\u0131z de\u011fi\u015fimi g\u00f6steren, erken B t\u00fcr\u00fc dev ve altdevlerden olu\u015fma bir gruptur. 2-7 saat aras\u0131nda de\u011ferlere sahip d\u00f6nemleri, d\u00f6nme ve\/veya \u00e7ift sistem hareketleri ile a\u00e7\u0131klanamayacak derecede k\u0131sad\u0131r ve tek ge\u00e7erli a\u00e7\u0131klama zonklama olmaktad\u0131r. Bu grubun, y\u0131ld\u0131z astrofizi\u011fi ve zonklama kuram\u0131 a\u00e7\u0131s\u0131ndan ayr\u0131cal\u0131kl\u0131 bir yeri vard\u0131r. \u00c7\u00fcnk\u00fc \u03b2 Cephei de\u011fi\u015fenlerinin zonklamalar\u0131n\u0131 do\u011furacak ve devam ettirecek teoriler yak\u0131n tarihe kadar tutarl\u0131 bir d\u00fczeye eri\u015fmemi\u015ftir ve kuramc\u0131lar\u0131 halen u\u011fra\u015ft\u0131rmaktad\u0131r.<\/p>\n

Patlayan de\u011fi\u015fenler ve y\u0131ld\u0131zlar<\/span><\/h2>\n

Anakol \u00f6ncesi y\u0131ld\u0131zlar (PMS), y\u0131ld\u0131zlararas\u0131 ortamdaki (Y\u0131ld\u0131zlararas\u0131 madde – Interstellar Medium \u2013 ISM) maddelerden yeni olu\u015fmu\u015f ve merkezlerinde n\u00fckleer tepkimeleri ba\u015flatacak s\u0131cakl\u0131\u011fa hen\u00fcz eri\u015fmemi\u015f y\u0131ld\u0131zlard\u0131r. Dolay\u0131s\u0131yla \u00e7ekimsel b\u00fcz\u00fclme sonucu s\u0131k\u0131\u015fan y\u0131ld\u0131z maddesinin sa\u011flad\u0131\u011f\u0131 enerji ile \u0131\u015f\u0131n\u0131m yapmaktad\u0131rlar. Fiziksel anlamda birbirinden pek de farkl\u0131 olmayan baz\u0131 y\u0131ld\u0131zlar ayr\u0131 alt gruplar olu\u015fturmu\u015flard\u0131r. \u00d6rne\u011fin RW Aur t\u00fcr\u00fc de\u011fi\u015fenler (GCVS de IS kodlu) ile T Tauri y\u0131ld\u0131zlar\u0131 olarak adland\u0131r\u0131lan (GCVS de INT kodlu) d\u00fc\u015f\u00fck k\u00fctleli PMS y\u0131ld\u0131zlar\u0131 aras\u0131nda fiziksel a\u00e7\u0131dan hi\u00e7bir fark yoktur. FU Orionis t\u00fcr\u00fc de\u011fi\u015fenler (GCVS de FU kodlu) ise evrimlerinin \u00f6zel bir safhas\u0131nda yer alan T Tauri y\u0131ld\u0131zlar\u0131d\u0131r. Bu t\u00fcrden de\u011fi\u015fenlere bazen genel olarak “Orion De\u011fi\u015fenleri” veya “Orion Pop\u00fclasyonu” da denmektedir. \u00c7\u00fcnk\u00fc Orion y\u0131ld\u0131z olu\u015fum b\u00f6lgesinde, bahsedilen t\u00fcm t\u00fcrlerden y\u0131ld\u0131z bulabilmek m\u00fcmk\u00fcnd\u00fcr. Bu y\u0131ld\u0131zlar\u0131n \u00e7o\u011fu halen olu\u015ftuklar\u0131 bulutsular\u0131n i\u00e7inde yer ald\u0131klar\u0131ndan “Bulutsu de\u011fi\u015fenleri” olarak da adland\u0131r\u0131lm\u0131\u015flard\u0131r.<\/p>\n

Bu yak\u0131n \u00e7ift y\u0131ld\u0131z sistemleri, birincil y\u0131ld\u0131z\u0131 etraf\u0131nda madde biriken bir beyaz c\u00fcce ve ikincil y\u0131ld\u0131z\u0131 d\u00fc\u015f\u00fck k\u00fctleli (g\u00fcne\u015fimizden biraz daha so\u011fuk) bir ana kol y\u0131ld\u0131z\u0131ndan olu\u015fur. \u0130kincilden akan maddenin zamanla birikip beyaz c\u00fccenin y\u00fczeyinde n\u00fckleer patlama yaratarak yanmas\u0131yla sistemin parlakl\u0131\u011f\u0131 bir ila birka\u00e7 y\u00fcz g\u00fcn s\u00fcresince 7 ila 16 kadir aras\u0131nda artar. Patlamadan sonra y\u0131ld\u0131z y\u0131llar i\u00e7inde yava\u015f yava\u015f eski parlakl\u0131\u011f\u0131na d\u00f6ner. Maksimum parlakl\u0131k civar\u0131nda y\u0131ld\u0131z\u0131n tayf\u0131 A ya da F dev y\u0131ld\u0131zlar\u0131 gibidir.<\/p>\n","protected":false},"excerpt":{"rendered":"

Kepler, y\u0131ld\u0131zlar ve tarih\u00e7esi D\u00fcnyan\u0131n her yerinde yo\u011fun bir \u015fekilde uzay\u0131 ke\u015ffetme \u00e7al\u0131\u015fmalar\u0131 devam ederken, yeni bir ke\u015fif de \u015eili’li astronomlardan geldi. Uzun zamand\u0131r g\u00f6ky\u00fcz\u00fc inceleme \u00e7al\u0131\u015fmalar\u0131 yapan bu grup, 9 adet de\u011fi\u015fken y\u0131ld\u0131z ke\u015ffetti. Peki nedir bu de\u011fi\u015fken y\u0131ld\u0131zlar? K\u0131sa ve anla\u015f\u0131l\u0131r bir \u015fekilde ifade etmek gerekirse; de\u011fi\u015fken y\u0131ld\u0131zlar, parlakl\u0131klar\u0131 zaman i\u00e7erisinde de\u011fi\u015fen y\u0131ld\u0131zlard\u0131r. […]<\/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-62814","post","type-post","status-publish","format-standard","hentry","category-astronomi"],"acf":[],"yoast_head":"\n9 De\u011fi\u015fken Y\u0131ld\u0131z Ke\u015ffettiler - Online Star Register<\/title>\n<meta name=\"description\" content=\"De\u011fi\u015fken y\u0131ld\u0131zlar yeni ke\u015fiflerle farkl\u0131 boyutlarda bilgileri beraberinde getiriyor\" \/>\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\/9-degisken-yildiz-kesfettiler\/\" \/>\n<meta property=\"og:locale\" content=\"tr_TR\" \/>\n<meta property=\"og:type\" content=\"article\" \/>\n<meta property=\"og:title\" content=\"9 De\u011fi\u015fken Y\u0131ld\u0131z Ke\u015ffettiler - 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