{"id":48898,"date":"2018-11-23T22:06:28","date_gmt":"2018-11-23T20:06:28","guid":{"rendered":"https:\/\/osr.org\/?p=48898\/"},"modified":"2023-07-24T14:01:14","modified_gmt":"2023-07-24T12:01:14","slug":"yildizlar-ve-tayflari","status":"publish","type":"post","link":"https:\/\/osr.org\/tr\/blog\/astronomi\/yildizlar-ve-tayflari\/","title":{"rendered":"Y\u0131ld\u0131zlar ve tayflar\u0131"},"content":{"rendered":"<p>Bir y\u0131ld\u0131z\u0131n kaderini yaln\u0131zca onun k\u00fctlesi belirledi\u011finden(b\u00fcy\u00fck oranda) buna ba\u011fl\u0131 olan s\u0131cakl\u0131k, yar\u0131\u00e7ap, renk, tayf \u00e7izgileri gibi bir\u00e7ok \u00f6zelli\u011fi de birbiriyle ilintilidir. Bu ili\u015fkilerden yola \u00e7\u0131kan Hertzsprung ve Russell, astronomide s\u0131k\u00e7a kulland\u0131\u011f\u0131m\u0131z HR Diyagram\u0131n\u0131 olu\u015fturdular.<\/p>\n<p>Ger\u00e7ekten de y\u0131ld\u0131z\u0131n bir\u00e7ok parametresinin birbirine ba\u011fl\u0131l\u0131\u011f\u0131ndan \u00f6t\u00fcr\u00fc \u00e7ok fazla \u015fey anlatt\u0131\u011f\u0131ndan bir y\u0131ld\u0131z\u0131 incelemek i\u00e7in bu diyagram olduk\u00e7a kullan\u0131\u015fl\u0131d\u0131r. Bize \u00f6\u011fretildi\u011fi gibi, HR diyagram\u0131 hakk\u0131nda saatlerce hatta g\u00fcnlerce konu\u015fmak m\u00fcmk\u00fcn.<\/p>\n<p>iyagramda bir\u00e7ok parametre ve y\u0131ld\u0131z t\u00fcr\u00fc g\u00f6r\u00fcn\u00fcyor. Yatay eksende verilen O, B, A, F, G, K, M de\u011ferleri az \u00f6nce bahsetti\u011fimiz tayf s\u0131n\u0131flar\u0131d\u0131r. Esprili bir \u015fekilde ak\u0131lda tutmak i\u00e7in s\u0131kl\u0131kla Oh Be A Fine Girl Kiss Me diye bahsedilir. Yine ayn\u0131 eksende renk \u00f6l\u00e7e\u011finin ve y\u00fczey s\u0131cakl\u0131\u011f\u0131n\u0131n da yer ald\u0131\u011f\u0131n\u0131 g\u00f6r\u00fcyoruz. Bu parametreler tayf t\u00fcr\u00fc ile do\u011frudan ili\u015fkili oldu\u011fundan yatay eksende bu \u00fc\u00e7 ifadeyi birden kullan\u0131yoruz. Dikey eksende kulland\u0131\u011f\u0131m\u0131z de\u011fer ise mutlak parlakl\u0131k (mutlak kadir) ya da \u0131\u015f\u0131tma g\u00fcc\u00fc.<\/p>\n<p>*Diyagramda k\u00f6\u015fegen gibi olan hatta, \u201canakol y\u0131ld\u0131zlar\u0131\u201d diyoruz. Bir y\u0131ld\u0131z \u00f6mr\u00fcn\u00fcn b\u00fcy\u00fck bir b\u00f6l\u00fcm\u00fcn\u00fc burada ge\u00e7irir. A\u015fa\u011f\u0131daki konuda ayr\u0131ca verilenler hari\u00e7 bahsetti\u011fimiz y\u0131ld\u0131zlar, anakol y\u0131ld\u0131zlar\u0131d\u0131r.<\/p>\n<h2><span style=\"color: #15acdf\">OBAFGKM ne demektir<\/span><\/h2>\n<p>Az \u00f6nce de ele ald\u0131\u011f\u0131m\u0131z gibi tayf t\u00fcrleri, renk ve y\u00fczey s\u0131cakl\u0131\u011f\u0131 ile do\u011frudan ili\u015fkilidir. Y\u00fczey s\u0131cakl\u0131\u011f\u0131 tayf \u00e7izgilerinde etkili oldu\u011fundan, tayf s\u0131n\u0131fland\u0131rmas\u0131nda yine do\u011frudan etkilidir. Bir y\u0131ld\u0131z\u0131n rengi de onun y\u00fczey s\u0131cakl\u0131\u011f\u0131 ile ilgili oldu\u011funa g\u00f6re bu parametreler birbiri ile i\u00e7 i\u00e7e ge\u00e7mi\u015f haldedir. Yine bu parametrelerden yola \u00e7\u0131karak y\u0131ld\u0131zlar\u0131 birbirleri ile ortak \u00f6zellik ta\u015f\u0131yacak \u015fekilde s\u0131n\u0131fland\u0131r\u0131yoruz. \u0130\u015fte bu OBAFGKM olarak ifade etti\u011fimiz harfler tayf s\u0131n\u0131flar\u0131d\u0131r.<\/p>\n<p>Ayn\u0131 zamanda kendi i\u00e7lerinde numaralar ile de alt gruplara ayr\u0131l\u0131r. \u00d6rne\u011fin biz G\u00fcne\u015f\u2019ten bahsederken G2 t\u00fcr\u00fc bir y\u0131ld\u0131z oldu\u011funu s\u00f6yleriz. O s\u0131n\u0131f\u0131 tayf t\u00fcr\u00fc diyagramda da g\u00f6r\u00fcld\u00fc\u011f\u00fc gibi mavi, olduk\u00e7a s\u0131cak y\u0131ld\u0131zlar\u0131 ifade ederken M\u2019ye do\u011fru gidildik\u00e7e y\u0131ld\u0131z\u0131n s\u0131cakl\u0131\u011f\u0131 azal\u0131yor ve rengi k\u0131rm\u0131z\u0131ya do\u011fru gidiyor. Alt gruplar\u0131 da dikkate alacak olursak soldan sa\u011fa bu s\u0131ralama O5\u2019ten ba\u015flayarak O6, O7, O8, O9, B0, B1, \u2026 , M7, M8 diye gidiyor. O5\u2019ten ba\u015fl\u0131yor olmas\u0131n\u0131n sebebi ise, olduk\u00e7a d\u00fc\u015f\u00fck olas\u0131l\u0131klarda olu\u015fup yine olduk\u00e7a k\u0131sa bir \u00f6mre sahip olan bu y\u0131ld\u0131zlar\u0131n g\u00f6zleminin nadir olmas\u0131 sebebiyle a\u00e7\u0131k bir u\u00e7 b\u0131rak\u0131lm\u0131\u015f olmas\u0131. Yani daha s\u0131cak bir y\u0131ld\u0131z\u0131n bulunmas\u0131 durumunda buraya bir s\u0131n\u0131f ekleyebilmek i\u00e7in O1\u2019den de\u011fil de O5\u2019ten ba\u015flatm\u0131\u015flar. Bunlara ek olarak her ne kadar y\u0131ld\u0131z olarak nitelendirilmeseler de, daha so\u011fuk olan kahverengi c\u00fcceleri ise ek bir tayf t\u00fcr\u00fc olarak L, T ve Y s\u0131n\u0131flar\u0131nda ele al\u0131yoruz. <\/p>\n<p>O tayf s\u0131n\u0131f\u0131ndan M tayf s\u0131n\u0131f\u0131na do\u011fru gidildik\u00e7e y\u00fczey s\u0131cakl\u0131\u011f\u0131, k\u00fctle, yar\u0131\u00e7ap ve \u0131\u015f\u0131tma g\u00fcc\u00fcn\u00fcn azald\u0131\u011f\u0131n\u0131 g\u00f6r\u00fcyoruz(*). Bu sayede bir y\u0131ld\u0131z\u0131n kaderini k\u00fctlesinin belirledi\u011fini daha a\u00e7\u0131k bir \u015fekilde anlam\u0131\u015f oluruz. E\u011fer k\u00fctle daha fazla ise k\u00fctle\u00e7ekim daha fazla, dolay\u0131s\u0131yla ya\u015fad\u0131\u011f\u0131 \u015fartlar daha serttir. Yak\u0131t\u0131n\u0131 daha h\u0131zl\u0131 harcar, daha k\u0131sa s\u00fcrede t\u00fcketir. Bu da y\u00fczey s\u0131cakl\u0131\u011f\u0131n\u0131n fazla, dolay\u0131s\u0131yla \u0131\u015f\u0131tma g\u00fcc\u00fcn\u00fcn de fazla olmas\u0131na sebep olur.<\/p>\n<p>O tayf t\u00fcr\u00fcnden bir y\u0131ld\u0131z\u0131n ya\u015f\u0131 1 milyon y\u0131l ile ifade edilirken, M tayf t\u00fcr\u00fcn\u00fcn y\u00fcz milyarca, hatta baz\u0131 u\u00e7 \u00f6rneklerde trilyonlarca y\u0131l ile ifade edilir. Bu sebeple istatistiksel olarak s\u0131cak ve vah\u015fi y\u0131ld\u0131zlar\u0131 daha nadiren g\u00f6r\u00fcr\u00fcz.<\/p>\n<h2><span style=\"color: #15acdf\">Tayf t\u00fcrleri<\/span><\/h2>\n<p>O tayf t\u00fcr\u00fc y\u0131ld\u0131zlar \u00e7ok y\u00fcksek y\u00fczey s\u0131cakl\u0131\u011f\u0131na ve dolay\u0131s\u0131yla \u00e7ok y\u00fcksek \u0131\u015f\u0131tma g\u00fcc\u00fcne sahiptirler. Y\u00fcksek y\u00fczey s\u0131cakl\u0131\u011f\u0131 sebebiyle enerjilerinin \u00e7o\u011funu mor\u00f6tede yay\u0131nlarlar (bkz. Wien Yasas\u0131). 55.000 K dereceye kadar y\u00fcksek y\u00fczey s\u0131cakl\u0131\u011f\u0131na sahip olabilirler.<\/p>\n<p>Hatta en u\u00e7 \u00f6rneklerden biri olan R136a1 y\u0131ld\u0131z\u0131 1,7 milyon y\u0131l ya\u015f\u0131nda, 265 G\u00fcne\u015f k\u00fctlesine ve 56.000 K y\u00fczey s\u0131cakl\u0131\u011f\u0131na sahip O tayf t\u00fcr\u00fcnden bir y\u0131ld\u0131z. Yar\u0131\u00e7ap\u0131 ise 29 G\u00fcne\u015f yar\u0131\u00e7ap\u0131 kadar. Bu da \u0131\u015f\u0131tma g\u00fcc\u00fcn\u00fc hesaplad\u0131\u011f\u0131m\u0131zda G\u00fcne\u015f\u2019ten tam 7.5 milyon kat fazla bir \u0131\u015f\u0131tma g\u00fcc\u00fcne sahip oldu\u011funu g\u00f6steriyor.<\/p>\n<p>Teorik olarak yap\u0131lan hesaplarda 150 G\u00fcne\u015f k\u00fctlesinin \u00fczerinde y\u0131ld\u0131z olu\u015fmamas\u0131n\u0131 bekliyoruz fakat bu y\u0131ld\u0131z\u0131n k\u00fctlesi neredeyse bunun iki kat\u0131. Son yap\u0131lan g\u00f6zlemler de do\u011fruluyor ki b\u00f6yle b\u00fcy\u00fck k\u00fctleli y\u0131ld\u0131zlar, iki b\u00fcy\u00fck k\u00fctleli y\u0131ld\u0131zlar\u0131n birle\u015fmesi sonucu olu\u015fabiliyor. Fakat zaten d\u00fc\u015f\u00fck bir olas\u0131l\u0131kla bulunma ihtimaline sahip b\u00fcy\u00fck k\u00fctleli y\u0131ld\u0131zlar\u0131n, b\u00f6yle y\u0131ld\u0131zlar\u0131 olu\u015fturmas\u0131 daha da nadir rastlanan bir olay. Yine baz\u0131 teorik modeller 150 G\u00fcne\u015f k\u00fctlesinden fazla k\u00fctleye sahip y\u0131ld\u0131zlar olu\u015fabilece\u011fini de s\u00f6yl\u00fcyor. Fakat bunlar\u0131n birer yakla\u015f\u0131m oldu\u011funu hat\u0131rlatmakta fayda var. G\u00f6zlemsel olarak elimizdeki en u\u00e7 noktalar bunlar. (bkz. Y\u0131ld\u0131zlarda minimum ve maksimum k\u00fctle)<\/p>\n<p>O tayf t\u00fcr\u00fcnden y\u0131ld\u0131zlar\u0131n ortalama \u00f6m\u00fcrleri milyon y\u0131l dolaylar\u0131ndad\u0131r. Ya\u015fam s\u00fcrelerinin b\u00f6yle k\u0131sa olmas\u0131n\u0131n sebebi, b\u00fcy\u00fck k\u00fctlelerinden \u00f6t\u00fcr\u00fc merkezdeki s\u0131cakl\u0131\u011f\u0131n ve bas\u0131nc\u0131n olduk\u00e7a y\u00fcksek olup yak\u0131t\u0131n\u0131 h\u0131zla t\u00fcketmesine sebep olmas\u0131d\u0131r. Bu t\u00fcr y\u0131ld\u0131zlar g\u00fc\u00e7l\u00fc ve h\u0131zl\u0131 ya\u015fay\u0131p, \u00e7abuk \u00f6l\u00fcrler. <\/p>\n<h2><span style=\"color: #15acdf\">B Tayf T\u00fcr\u00fc<\/span><\/h2>\n<p>Olduk\u00e7a s\u0131cak ve mavi y\u0131ld\u0131zlard\u0131r. O tayf t\u00fcr\u00fcne g\u00f6re biraz daha m\u00fctevazi bir ya\u015fam s\u00fcrmelerine ra\u011fmen hala olduk\u00e7a \u201cg\u00fc\u00e7l\u00fc\u201d y\u0131ld\u0131zlard\u0131r. Bu sebeple ya\u015fam s\u00fcreleri O tayf t\u00fcr\u00fcnden fazla olsa da yine de olduk\u00e7a k\u0131sad\u0131r.<\/p>\n<p>En \u00e7ok tan\u0131d\u0131\u011f\u0131m\u0131z y\u0131ld\u0131zlardan Rigel (\u03b2 Orionis) bu tayf t\u00fcr\u00fcnden, B8 s\u0131n\u0131f\u0131 bir mavi s\u00fcperdevdir. Yakla\u015f\u0131k 8 milyon ya\u015f\u0131nda, 12.000K y\u00fczey s\u0131cakl\u0131\u011f\u0131na, 80 G\u00fcne\u015f yar\u0131\u00e7ap\u0131na, 21 G\u00fcne\u015f k\u00fctlesine ve G\u00fcne\u015f\u2019in 120.000 kat\u0131 \u0131\u015f\u0131tma g\u00fcc\u00fcne sahiptir.<\/p>\n<h2><span style=\"color: #15acdf\">A Tayf T\u00fcr\u00fc<\/span><\/h2>\n<p>O ve B tayf t\u00fcr\u00fcnde g\u00f6re g\u00f6ky\u00fcz\u00fcnde \u00e7\u0131plak g\u00f6zle g\u00f6rmeye al\u0131\u015f\u0131k oldu\u011fumuz pop\u00fcler daha fazla y\u0131ld\u0131z\u0131 bar\u0131nd\u0131r\u0131r. Beyaz\u0131ms\u0131 mavimsi renktedirler. A0 tayf t\u00fcr\u00fcnden, yaz \u00fc\u00e7geninin bir par\u00e7as\u0131 olan Vega yakla\u015f\u0131k 825 milyon y\u0131l ya\u015f\u0131ndad\u0131r. 2.1 G\u00fcne\u015f k\u00fctlesine, 2.5 G\u00fcne\u015f yar\u0131\u00e7ap\u0131na ve G\u00fcne\u015f\u2019in 40 kat\u0131 \u0131\u015f\u0131tma g\u00fcc\u00fcne sahiptir. Bu durum O ve B tayf t\u00fcr\u00fc ile k\u0131yaslay\u0131nca olduk\u00e7a s\u0131radan g\u00f6r\u00fcn\u00fcyor. Y\u00fczey s\u0131cakl\u0131\u011f\u0131 ise ortalama 9.500 K. Vega hakk\u0131nda daha detayl\u0131 bilgi i\u00e7in bu makalemize bakabilirsiniz.<\/p>\n<h2><span style=\"color: #15acdf\">F Tayf T\u00fcr\u00fc<\/span><\/h2>\n<p>Renkleri beyaz olan F tayf t\u00fcr\u00fcnden y\u0131ld\u0131zlardan g\u00f6ky\u00fcz\u00fcn\u00fcn tan\u0131d\u0131\u011f\u0131m\u0131z \u00fcyesi Procyon. K\u00fc\u00e7\u00fck k\u00f6pek tak\u0131m y\u0131ld\u0131z\u0131n\u0131n en parlak \u00fcyesi Procyon(A) F5 tayf t\u00fcr\u00fcnden bir y\u0131ld\u0131zd\u0131r. 3 milyar y\u0131l ya\u015f\u0131nda ve 6.500 K y\u00fczey s\u0131cakl\u0131\u011f\u0131na sahiptir. Ayn\u0131 zamanda 1,42 G\u00fcne\u015f k\u00fctlesinde, 2 G\u00fcne\u015f yar\u0131\u00e7ap\u0131nda ve G\u00fcne\u015f\u2019in \u0131\u015f\u0131tma g\u00fcc\u00fcn\u00fcn 7 kat\u0131 bir \u0131\u015f\u0131tma g\u00fcc\u00fcne sahip.<br \/>\nG Tayf T\u00fcr\u00fc<\/p>\n<p>G\u00fcne\u015f\u2019imizin de dahil oldu\u011fu bu tayf t\u00fcr\u00fcnden y\u0131ld\u0131zlar sar\u0131ms\u0131 renge sahiptirler. G\u00fcne\u015f\u2019in ya\u015f\u0131 4.6 milyar(\u00f6mr\u00fc yakla\u015f\u0131k 10 milyar), y\u00fczey s\u0131cakl\u0131\u011f\u0131 ise yakla\u015f\u0131k 5780 K\u2019dir. Di\u011fer tayf s\u0131n\u0131flar\u0131n\u0131 a\u00e7\u0131klarken verdi\u011fimiz yar\u0131\u00e7ap, k\u00fctle ve \u0131\u015f\u0131tma g\u00fcc\u00fc de\u011ferleri G\u00fcne\u015f cinsinden idi. <\/p>\n<p>G\u00f6ky\u00fcz\u00fcn\u00fcn bir tan\u0131d\u0131\u011f\u0131m\u0131z \u00fcyesi daha olan Pollux K0 tayf t\u00fcr\u00fcnden bir y\u0131ld\u0131z. G\u00fcne\u015f\u2019ten nispeten daha so\u011fuk y\u0131ld\u0131zlar. Pollux 2 G\u00fcne\u015f k\u00fctlesine, 8.8 G\u00fcne\u015f yar\u0131\u00e7ap\u0131na ve G\u00fcne\u015f\u2019in 43 kat\u0131 bir \u0131\u015f\u0131tma g\u00fcc\u00fcne sahip. Ya\u015f\u0131 ise yaln\u0131zca 724 milyon y\u0131l.<\/p>\n<p>M tayf t\u00fcr\u00fcnden y\u0131ld\u0131zlar anakol y\u0131ld\u0131zlar\u0131n\u0131n %76\u2019l\u0131k bir k\u0131sm\u0131n\u0131 olu\u015fturur. D\u00fc\u015f\u00fck y\u00fczey s\u0131cakl\u0131kl\u0131klar\u0131 ve dolay\u0131s\u0131yla \u0131\u015f\u0131tma g\u00fc\u00e7leri sebebiyle kendilerini daha az belli ederler. Hatta anakol evresine ait bilinen en parlak M tayf t\u00fcr\u00fc y\u0131ld\u0131z 6.6 kadir oldu\u011fundan \u00f6t\u00fcr\u00fc hi\u00e7birini \u00e7\u0131plak g\u00f6zle g\u00f6remeyiz. <\/p>\n","protected":false},"excerpt":{"rendered":"<p>Bir y\u0131ld\u0131z\u0131n kaderini yaln\u0131zca onun k\u00fctlesi belirledi\u011finden(b\u00fcy\u00fck oranda) buna ba\u011fl\u0131 olan s\u0131cakl\u0131k, yar\u0131\u00e7ap, renk, tayf \u00e7izgileri gibi bir\u00e7ok \u00f6zelli\u011fi de birbiriyle ilintilidir. Bu ili\u015fkilerden yola \u00e7\u0131kan Hertzsprung ve Russell, astronomide s\u0131k\u00e7a kulland\u0131\u011f\u0131m\u0131z HR Diyagram\u0131n\u0131 olu\u015fturdular. Ger\u00e7ekten de y\u0131ld\u0131z\u0131n bir\u00e7ok parametresinin birbirine ba\u011fl\u0131l\u0131\u011f\u0131ndan \u00f6t\u00fcr\u00fc \u00e7ok fazla \u015fey anlatt\u0131\u011f\u0131ndan bir y\u0131ld\u0131z\u0131 incelemek i\u00e7in bu diyagram olduk\u00e7a kullan\u0131\u015fl\u0131d\u0131r. [&hellip;]<\/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-48898","post","type-post","status-publish","format-standard","hentry","category-astronomi"],"acf":[],"yoast_head":"<!-- This site is optimized with the Yoast SEO plugin v26.5 - https:\/\/yoast.com\/wordpress\/plugins\/seo\/ -->\n<title>Y\u0131ld\u0131zlar ve tayflar\u0131 - Online Star Register<\/title>\n<meta name=\"description\" content=\"Her y\u0131ld\u0131z\u0131n bir tayf\u0131 vard\u0131r ve hepsi de farkl\u0131 t\u00fcrlerde tayflara sahiptir\" \/>\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\/yildizlar-ve-tayflari\/\" \/>\n<meta property=\"og:locale\" content=\"tr_TR\" \/>\n<meta property=\"og:type\" content=\"article\" \/>\n<meta property=\"og:title\" content=\"Y\u0131ld\u0131zlar ve tayflar\u0131 - 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