{"id":13435,"date":"2020-09-23T13:47:15","date_gmt":"2020-09-23T10:47:15","guid":{"rendered":"https:\/\/hayrettinkagnici.com\/?p=13435"},"modified":"2021-12-04T13:49:42","modified_gmt":"2021-12-04T10:49:42","slug":"cosmos-ve-samanyolu","status":"publish","type":"post","link":"https:\/\/hayrettinkagnici.com\/tr\/cosmos-ve-samanyolu\/","title":{"rendered":"Samanyolu Galaksisi ve Cosmos"},"content":{"rendered":"<p>&nbsp;<\/p>\n<p>Cosmos, i\u00e7inde d\u00fcnyam\u0131z ve g\u00fcne\u015f sistemi olan Samanyolu galaksisi gibi 2 trilyon ba\u015fka galaksilerin ayr\u0131ca uzay dedi\u011fimiz b\u00fcy\u00fck bo\u015fluklar\u0131, rakamlara s\u0131\u011fmayacak kadar \u00e7ok y\u0131ld\u0131z ve gezegenlerin oldu\u011fu devasa boyutta bir yerdir.<\/p>\n<p>Samanyolu galaksisi bile \u015fu anda 2500 gezegenin isimlendirilerek takip edildi\u011fi ancak toplam 3,2 milyon gezegen ve 50 milyar y\u0131ld\u0131z\u0131n oldu\u011fu bir alan. Havan\u0131n a\u00e7\u0131k, bulutsuz ve yeni ay evrelerinde yani ay\u0131n olmad\u0131\u011f\u0131 veya ince hilal d\u00f6nemlerinde g\u00fcney istikametinde g\u00f6rd\u00fc\u011f\u00fcm\u00fcz, genelde samanyolu diye bilinen \u201cg\u00f6k ada\u201d milyonlarca y\u0131ld\u0131z\u0131n k\u00fctlesel \u00e7ekim kuvveti ile bir arada k\u00fcmeleni\u015f halidir. \u00a0Samanyolu galaksisinde milyarlarca olan g\u00f6k ada y\u0131ld\u0131z k\u00fcmelerinden ancak bir tanesi astronomik g\u00f6zlem olarak ya\u015fad\u0131\u011f\u0131m\u0131z gezegenden g\u00f6r\u00fclebilmektedir. M\u00d6 den beri izlenen bu y\u0131ld\u0131z k\u00fcmesi Osmanl\u0131 da \u201cKehke\u015fan\u201d, Uzak Do\u011fuda \u201cg\u00fcm\u00fc\u015f yolu\u201d, Kuzey Afrika ve Ortado\u011fu \u00fclkelerinde \u201chac yolu\u201d veya \u201ckral yolu\u201d olarak bilinir. En yayg\u0131n olarak \u201cmilky way\u201d s\u00fct yolu olarak bilinen y\u0131ld\u0131z k\u00fcmesi, dilimizde de i\u00e7inde bulundu\u011fumuz galaksinin ad\u0131 olan samanyolu y\u0131ld\u0131z k\u00fcmesi olarak kullan\u0131l\u0131r.<\/p>\n<p>Mitolojik olarak, Yunan mitolojisinde, baba tanr\u0131 Zeus, \u00f6l\u00fcml\u00fc bir kad\u0131n ile birlikte olur ve o\u011flu Roma mitolojisinde Herk\u00fcl olarak bilinen Herakles d\u00fcnyaya gelir. O\u011flunu \u00f6l\u00fcms\u00fcz k\u0131lmak i\u00e7in bir gece ana tanr\u0131\u00e7a Hera\u2019n\u0131n g\u00f6\u011fs\u00fcne s\u00fct emmesi i\u00e7in b\u0131rak\u0131r. Bir s\u00fcre sonra uyanan Hera, g\u00f6\u011fs\u00fcnde tan\u0131mad\u0131\u011f\u0131 birini g\u00f6r\u00fcnce f\u0131rlat\u0131r atar, g\u00f6\u011fs\u00fcnden bo\u015falan s\u00fctler de\u00a0g\u00f6ky\u00fcz\u00fcne do\u011fru f\u0131\u015fk\u0131r\u0131r ve s\u00fct yolu dedi\u011fimiz olay meydana gelir.<\/p>\n<p>\u0130lk olarak, antik \u00e7a\u011f d\u00f6nemlerinde M\u00d6. 470-350) y\u0131llar\u0131nda Yunan filozof Demokritus taraf\u0131ndan g\u00f6zlenen y\u0131ld\u0131z k\u00fcmesi, sonralar\u0131 \u0130skenderiye k\u00fct\u00fcphanesi Platon okulunda filozof Aristo (M\u00d6. 384-229 taraf\u0131ndan da g\u00f6zlenip uzun s\u00fcre incelenmi\u015f ve ilk olarak birbirine yak\u0131n \u00e7ok say\u0131da y\u0131ld\u0131zlardan olu\u015ftan y\u0131ld\u0131zlar k\u00fcmesi oldu\u011funu a\u00e7\u0131klam\u0131\u015ft\u0131r. Zaman i\u00e7inde bir\u00e7ok g\u00f6kbilimci bu konuda \u00e7al\u0131\u015fmalar yapm\u0131\u015f, ilk olarak 1610 y\u0131l\u0131nda filozof Galile bunlar\u0131n birbirine ba\u011fl\u0131 \u00e7ok say\u0131da y\u0131ld\u0131zlardan olu\u015fan k\u00fcme oldu\u011fu sa\u00e7\u0131klam\u0131\u015ft\u0131r. Son olarak 1750 y\u0131l\u0131nda \u0130ngiliz bilim adam\u0131 Thomas Wright bunlar\u0131n \u00e7ok say\u0131da y\u0131ld\u0131z\u0131n b\u00fcy\u00fck k\u00fctlesel \u00e7ekim kuvveti ile birbirine yak\u0131n y\u0131ld\u0131zdan olu\u015fan y\u0131ld\u0131zlar k\u00fcmesi \u201cg\u00f6k ada\u201d oldu\u011funu kan\u0131tlam\u0131\u015ft\u0131r.<\/p>\n<p>Samanyolu galaksisi, evrendeki \u00e7ok say\u0131da galaksiden biri olup, galaksi i\u00e7inde en az 200-400 milyar \u00a0y\u0131ld\u0131z oldu\u011fu ve milyonlarca g\u00f6k ada bulundu\u011fu tespit edilmi\u015ftir. G\u00f6k adan\u0131n merkezine do\u011fru \u00e7ok say\u0131da birbirine yak\u0131n, merkezden uzakla\u015ft\u0131k\u00e7a iki tarafa uzayan kollar \u015feklinde daha seyrek y\u0131ld\u0131zlar bulunmaktad\u0131r.\u00a0 G\u00f6kada\u2019ya ba\u011fl\u0131 \u00f6m\u00fcrleri biten \u0131\u015f\u0131klar\u0131 s\u00f6nmeye ba\u015flayan y\u0131ld\u0131zlar vard\u0131r ve bunlara \u201cc\u00fcce\u201d y\u0131ld\u0131zlar denir.<\/p>\n<p>G\u00fcne\u015f, Samanyolu galaksi merkezinden 28 bin \u0131\u015f\u0131k y\u0131l\u0131 uzakl\u0131ktad\u0131r ve cosmos b\u00fct\u00fcnl\u00fc\u011f\u00fcn i\u00e7inde 2 trilyon galaksi oldu\u011fu biliniyor.<\/p>\n<p>Buna g\u00f6re galaksimiz hakk\u0131nda baz\u0131 de\u011ferlere bakarsak;<\/p>\n<p>&nbsp;<\/p>\n<ul>\n<li>cosmos konular\u0131nda genelde \u0131\u015f\u0131k y\u0131l\u0131 ifadesi kullan\u0131l\u0131r, \u0131\u015f\u0131k y\u0131l\u0131 zaman birimi de\u011fil mesafe \u00f6l\u00e7\u00fcs\u00fcd\u00fcr. I\u015f\u0131\u011f\u0131n h\u0131z\u0131 300.000 km\/saniye oldu\u011funa g\u00f6re bir \u0131\u015f\u0131k y\u0131l\u0131 9,5 trilyon km. uzakl\u0131k demektir.<\/li>\n<li>B\u00fcy\u00fck bir disk \u015feklinde oldu\u011fu kabul edilen Samanyolu galaksinin kal\u0131nl\u0131\u011f\u0131 10 \u0131\u015f\u0131k y\u0131l\u0131, \u00e7ap\u0131 100 bin \u0131\u015f\u0131k y\u0131l\u0131 ve 3,5 milyar ya\u015f\u0131ndad\u0131r.<\/li>\n<li>D\u00fcnyan\u0131n samanyolu galaksisinin i\u00e7indeki y\u00f6r\u00fcngesini 200 milyon \u0131\u015f\u0131k y\u0131l\u0131nda tamaml\u0131yor.<\/li>\n<li>Samanyolu galaksisinde bulunan d\u00fcnyan\u0131n kendi etraf\u0131nda d\u00f6n\u00fc\u015f h\u0131z\u0131; 1.627 km\/saat<\/li>\n<li>D\u00fcnyan\u0131n g\u00fcne\u015f etraf\u0131ndaki d\u00f6nme h\u0131z\u0131, 107.627 km\/saat<\/li>\n<li>G\u00fcne\u015fin galaksi i\u00e7indeki hareket h\u0131z\u0131 930.000 km\/saat<\/li>\n<li>Samanyolu Galaksisinde; 200 milyar y\u0131ld\u0131z ve g\u00fcne\u015f sistemi oldu\u011fu kabul bilindi\u011fine g\u00f6re, her bir y\u0131ld\u0131z\u0131n\u0131n en az bir ve daha fazla gezegene sahip oldu\u011fu d\u00fc\u015f\u00fcn\u00fcl\u00fcrse Samanyolu galaksisinde 3,2 trilyon gezegen kabul edilmektedir. Bunlardan sadece 2500 gezegen isimlendirilmi\u015ftir.<\/li>\n<li>Yap\u0131lan en son ara\u015ft\u0131rmalar, \u00e7ap\u0131 100-120 bin \u0131\u015f\u0131k y\u0131l\u0131 olan Samanyolu galakside, D\u00fcnya ile ayn\u0131 b\u00fcy\u00fckl\u00fckte en az 17 milyar gezegen bulundu\u011funu g\u00f6stermi\u015ftir.<\/li>\n<li>Cosmos da 2 trilyon galaksi oldu\u011fu tespit edilmi\u015ftir.<\/li>\n<\/ul>\n<p>Astronomi de mesafeler, metrik sistemin d\u0131\u015f\u0131nda birimler ile ifade edilir;<\/p>\n<ul>\n<li>1Parsek, 3, 26 \u0131\u015f\u0131k y\u0131l\u0131 veya 30 trilyon km.<\/li>\n<li>1 AU (Astronomik Unit ), 150 milyon km. Bu de\u011fer, d\u00fcnyan\u0131n merkezinden g\u00fcne\u015fin merkezine olan mesafedir.<\/li>\n<li>Ekvator \u00e7evresi 40,000km olan d\u00fcnyam\u0131z\u0131n aya olan uzakl\u0131\u011f\u0131 375,000 km dir.<\/li>\n<\/ul>\n<p>D\u00fcnya, G\u00fcne\u015f Sistemi&#8217;nde G\u00fcne\u015f&#8217;e en yak\u0131n \u00fc\u00e7\u00fcnc\u00fc gezegen olup \u015fu an i\u00e7in \u00fczerinde ya\u015fam ve s\u0131v\u0131 su bar\u0131nd\u0131rd\u0131\u011f\u0131 bilinen tek astronomik cisimdir. Radyometrik tarihleme ve di\u011fer kan\u0131tlara g\u00f6re 4,5 milyar y\u0131ldan fazla s\u00fcre \u00f6nce olu\u015fmu\u015ftur<\/p>\n<p>&nbsp;<\/p>\n<ul>\n<li>D\u00fcnya\/\u00c7evresi 40.075 km<\/li>\n<li>Ya\u015f\u0131: D\u00fcnya&#8217;n\u0131n ya\u015f\u0131n\u0131n yakla\u015f\u0131k 4,54 milyar y\u0131l (4,54\u00d710<sup>9<\/sup> y\u0131l)<\/li>\n<li>Yar\u0131\u00e7ap: 6.371 km<\/li>\n<li>Ortalama y\u00f6r\u00fcnge h\u0131z\u0131: 29,78 km\/s; (107200 km\/sa; 66600 mph)<\/li>\n<li>Ekvatoral d\u00f6nme h\u0131z\u0131: 0,4651 km\/s; (1674,4 km\/sa; 1040,4 mph)<\/li>\n<li>Ortalama yar\u0131\u00e7ap: 6371,0 km<\/li>\n<li>Y\u00f6r\u00fcnge periyodu: 365,256363004 d; (1,00001742096 yr)<\/li>\n<li>Ekvatoral yar\u0131\u00e7ap: 6378,1 km (3963,2 mi)<\/li>\n<li>G\u00fcne\u015fe uzakl\u0131\u011f\u0131: 149.600.000 km<\/li>\n<li>Alan: 148.900.000 km\u00b2<\/li>\n<li>K\u00fctle: 5,972X10<sup>24<\/sup> kg<\/li>\n<\/ul>\n<p>&nbsp;<\/p>\n<p>Aya ula\u015f\u0131mda \u015fimdiye kadar giden en h\u0131zl\u0131 insans\u0131z uzay arac\u0131 2016 y\u0131l\u0131nda yollanan New Horinon 45,000 km \/saat ile ay\u0131n yan\u0131ndan ge\u00e7mi\u015fti, bug\u00fcn insans\u0131z uydu arac\u0131 olarak ula\u015f\u0131lan en y\u00fcksek h\u0131z 50,000 km\/saat. Bu h\u0131zla devaml\u0131 gidersek bizden 1 \u0131\u015f\u0131k y\u0131l\u0131 mesafede olan bir gezegene ancak 22,000 y\u0131l sonra ula\u015fabiliyoruz. Nasa\u2019n\u0131n h\u0131z olarak ula\u015fmak istedi\u011fi hedef ise 100,000 km\/saat. Bu h\u0131za ula\u015f\u0131ld\u0131\u011f\u0131nda 111,000 y\u0131lda 1 \u0131\u015f\u0131k y\u0131l\u0131 mesafeyi kat etmi\u015f olaca\u011f\u0131z.<\/p>\n<p>&nbsp;<\/p>\n<ul>\n<li>Devaml\u0131 hareket eden y\u0131ld\u0131z ve gezegenlerin de\u011fi\u015fen mesafe ve konumlar\u0131n\u0131 \u00f6l\u00e7mek i\u00e7in d\u00fcnyada bulundu\u011fumuz yer ile y\u0131ld\u0131z aras\u0131ndaki a\u00e7\u0131y\u0131 bilmemiz gerekir. Ancak bu kadar uzakl\u0131kta a\u00e7\u0131sal de\u011feri \u00f6l\u00e7mek kolay olmayaca\u011f\u0131 i\u00e7in 1 derecenin 3600 de biri olan arc\/sec veya yay\/saniye a\u00e7\u0131 birimi kullan\u0131l\u0131r.<\/li>\n<li>Uzay da k\u00fctle birimi olarak g\u00fcne\u015fin k\u00fctlesi, birim k\u00fctle olarak dikkate al\u0131n\u0131r. G\u00fcne\u015fin k\u00fctlesi 1 Nonilyon kg, yani 2&#215;10 <sup>30<\/sup> kg d\u0131r. Di\u011fer y\u0131ld\u0131zlar\u0131n k\u00fctle birimi i\u00e7inde g\u00fcne\u015fin k\u00fctle birimi dikkate al\u0131n\u0131r.<\/li>\n<li>G\u00fcne\u015fin k\u00fctlesi, d\u00fcnyan\u0131n k\u00fctlesinin 1,300 milyon kat\u0131d\u0131r ve hacim olarak da 330,000 kat\u0131d\u0131r.<\/li>\n<li>Y\u0131ld\u0131zlar\u0131n parlakl\u0131\u011f\u0131 \u00e7ok \u00f6nemlidir ve \u201ckadir\u201d birimi ile tarif edilir. En parlak y\u0131ld\u0131z\u0131n parlakl\u0131k birimi 6 Kadirdir, buradan logaritmik olarak en s\u00f6n\u00fck y\u0131ld\u0131za kadar derecelendirilir. Referans olarak da Polaris\u2019in, (kutup y\u0131ld\u0131z\u0131) parlakl\u0131k de\u011feri dikkate al\u0131n\u0131r.<\/li>\n<li>Samanyolu galaksi 100,000 \u0131\u015f\u0131k y\u0131l\u0131 b\u00fcy\u00fckl\u00fckte, yani 100,000x 10 trilyon km=10<sup>17<\/sup> km. dir<\/li>\n<li>Evrenin ya\u015f\u0131 13,8milyar d\u0131r. Yani Big Bang b\u00fcy\u00fck patlama 13,8 milyar y\u0131l \u00f6nce meydana gelmi\u015f.<\/li>\n<li>G\u00fcne\u015fin \u00f6mr\u00fcn\u00fcn 10 milyar y\u0131l oldu\u011fu kabul ediliyor, kalan s\u00fcre ise 4,5 milyar y\u0131l. Yani bu s\u00fcre sonunda g\u00fcne\u015f \u0131\u015f\u0131\u011f\u0131n\u0131 ve g\u00fcc\u00fcn\u00fc kaybetmeye ba\u015flayacak.<\/li>\n<li>Y\u0131ld\u0131zlar \u00f6m\u00fcrlerini tamamlay\u0131nca \u00f6nce s\u00f6n\u00fck \u0131\u015f\u0131k yayarlar, bu duruma \u201cbeyaz c\u00fcce\u201d, \u0131\u015f\u0131klar\u0131n\u0131 tamamen kaybedince \u201csiyah c\u00fcce\u201d ad\u0131n\u0131 al\u0131r.<\/li>\n<li>Tarihte ilk ke\u015ffedilen y\u0131ld\u0131z Sirus y\u0131ld\u0131z\u0131d\u0131r. Sirus y\u0131ld\u0131z\u0131 birbiri etraf\u0131nda d\u00f6nem iki y\u0131ld\u0131zdan meydana gelir. Sirus A ve S\u0131r\u0131B. Sirus B beyaz c\u00fcce yani s\u00f6nmekte olan y\u0131ld\u0131z, Sirus A g\u00fcne\u015ften 2 defa daha b\u00fcy\u00fck oldu\u011fu i\u00e7in g\u00fcne\u015ften 25 defa daha fazla enerji al\u0131r ve bu nedenle en parlak y\u0131ld\u0131z olarak g\u00f6z\u00fcyor. Sirus A ya\u015fam \u00f6mr\u00fcn\u00fc olan 2 milyar y\u0131l\u0131n b\u00fcy\u00fck k\u0131sm\u0131n\u0131 tamamlam\u0131\u015f, kalan 500 y\u0131l sonra dan itibaren beyaz c\u00fcce olmaya ba\u015flayacak ve giderek kaybolacak ve biz 500 milyon y\u0131l sonra g\u00f6remeyece\u011fiz.<\/li>\n<\/ul>\n<p>&nbsp;<\/p>\n<p><strong><em>Evrenin Kalp At\u0131\u015flar\u0131: Pulsarlar (Atarcalar) ve &#8220;Sesleri&#8221;;<\/em><\/strong><\/p>\n<p>Pulsarlar, kalp at\u0131\u015flar\u0131 gibi muntazam ritimlerle uzaya radyo dalgalar\u0131 g\u00f6nderen n\u00f6tron y\u0131ld\u0131zlar\u0131d\u0131r. Latincede \u201cpulsate\u201d kelimesinden gelen pulsar kalp gibi atan\u201d anlam\u0131na gelir. Y\u0131ld\u0131zlar k\u00fctlelerine g\u00f6re evrilirler. Bir y\u0131ld\u0131z\u0131n k\u00fctlesi ne kadar k\u00fc\u00e7\u00fckse s\u0131cakl\u0131\u011f\u0131 da bir o kadar d\u00fc\u015f\u00fck olur; \u00f6mr\u00fc de o kadar uzun olur. K\u00fctlesi \u00e7ok b\u00fcy\u00fck olan y\u0131ld\u0131zlar ise \u00f6m\u00fcrleri \u00e7ok k\u0131sad\u0131r. Bir y\u0131ld\u0131z\u0131n k\u00fctlesi ne kadar b\u00fcy\u00fckse s\u0131cakl\u0131\u011f\u0131 ve \u00e7ap\u0131 da o kadar b\u00fcy\u00fckt\u00fcr ancak \u00f6mr\u00fc \u00e7ok ihti\u015faml\u0131 bir \u015fekilde son bulur.<\/p>\n<p>B\u00fcy\u00fck k\u00fctleli y\u0131ld\u0131zlar\u0131n y\u00fczeyinde olu\u015fan n\u00fckleer reaksiyonlar, \u00e7ekirdekten d\u0131\u015fa do\u011fru bas\u0131n\u00e7 kuvveti olu\u015fturur, bu kuvve,t k\u00fctle \u00e7ekim kuvveti dengelenir. Ancak n\u00fckleer yak\u0131tlar\u0131n\u0131 biten y\u0131ld\u0131zlar\u0131n hidrostatik dengeleri bozulur.\u00a0 Bu durumda dev y\u0131ld\u0131z\u0131n k\u00fctle \u00e7ekim kuvveti, d\u0131\u015fa bas\u0131n\u00e7 kuvvetine bask\u0131n hale gelir ve y\u0131ld\u0131z kendi k\u00fctle \u00e7ekimi alt\u0131nda \u00e7\u00f6kmeye ba\u015flar. Unutmay\u0131n devasa b\u00fcy\u00fckl\u00fckte bir y\u0131ld\u0131zdan bahsediyoruz. K\u00fctle \u00e7ekim kuvveti o kadar y\u00fcksektir ki atomun yap\u0131 ta\u015flar\u0131 olan proton ve elektronlar dahi bundan etkilenir. Proton ve elektronlar bu \u00e7ekim kuvvetine kar\u015f\u0131 koyamaz ve bir araya gelip n\u00f6tronlar\u0131 olu\u015ftururlar. Tamam\u0131yla n\u00f6tronlardan olu\u015fmu\u015f bu y\u0131ld\u0131z \u00e7ekirde\u011fi, \u00e7\u00f6kme nedeniyle a\u00e7\u0131sal momentumu gere\u011fi giderek artan h\u0131zla d\u00f6nmeye ba\u015flar. Y\u00fcksek s\u0131cakl\u0131\u011fa ve manyetik alana sahip olan n\u00f6tron y\u0131ld\u0131z\u0131, manyetik kutuplar\u0131ndan uzaya do\u011fru X-\u0131\u015f\u0131n\u0131 sa\u00e7ar. Meydana gelen bu yap\u0131ya ise pulsar (atarca) denir.<\/p>\n<p>Pulsarlar, \u00e7ok y\u00fcksek h\u0131zlarda kendi etraf\u0131nda d\u00f6nerken, sahip oldu\u011fu manyetik alan nedeniyle kutuplar\u0131ndan uzaya do\u011fru par\u00e7ac\u0131k sa\u00e7an (X-\u0131\u015f\u0131n\u0131) n\u00f6tron y\u0131ld\u0131zlar\u0131d\u0131r. 10-15 km yar\u0131\u00e7apl\u0131 bir pulsar, yakla\u015f\u0131k 1 milyon km yar\u0131\u00e7apl\u0131 g\u00fcne\u015ften \u00e7ok daha y\u00fcksek oranda m\u0131knat\u0131slanm\u0131\u015f \u00f6zg\u00fcl k\u00fctleye sahiptir ve \u00f6zg\u00fcl k\u00fctlesi o derece b\u00fcy\u00fckt\u00fcr ki bir \u00e7ay ka\u015f\u0131\u011f\u0131 n\u00f6tron y\u0131ld\u0131z\u0131 yakla\u015f\u0131k bir milyon ton a\u011f\u0131rl\u0131\u011f\u0131ndad\u0131r. Meydana gelen manyetik \u0131\u015f\u0131man\u0131n par\u00e7ac\u0131klar\u0131 kutuplar\u0131ndan d\u0131\u015far\u0131 evrene sa\u00e7\u0131l\u0131r ve bu radyasyon at\u0131mlar\u0131 (pulse-darbe) denk gelip d\u00fcnyaya ula\u015ft\u0131k\u00e7a yery\u00fcz\u00fcnden duyulabilir. Bu sesler PSR Pulse Sourse of Radio olarak adland\u0131r\u0131l\u0131r ve her pulsar\u0131n da kaydedilen sesleri farkl\u0131d\u0131r. Bu seslerin analizi ile o pulsar\u0131n konumlar\u0131 hakk\u0131nda bilgiler elde edilir.\u00a0 \u00d6zel cihazlarla dinlenebilen bu sesler asl\u0131nda ger\u00e7ek anlamda &#8220;ses dalgas\u0131&#8221; de\u011fildir, radyo dalgalar\u0131n\u0131n sese dalgalar\u0131na d\u00f6n\u00fc\u015ft\u00fcr\u00fclerek bizim duyma aral\u0131\u011f\u0131m\u0131za indirgenmi\u015f halidir. Bu seslere \u201cp\u0131lsarlar\u0131n kalp at\u0131\u015f\u0131\u201d denir.<\/p>\n<p>Hepimizin duydu\u011fu, zaman zaman \u00fczerinde konu\u015ftu\u011fumuz \u00f6rnekleme yapt\u0131\u011f\u0131m\u0131z cosmosun en \u00f6nemli derinliklerinden olan <strong><em>\u201ckara delik\u201d<\/em><\/strong> ve <strong><em>\u201cbeyaz delik\u201d<\/em><\/strong> nedir?<\/p>\n<p>&nbsp;<\/p>\n<p><strong><em>Kara delik;<\/em><\/strong><\/p>\n<p>Kara delik, astro fizikte, \u00e7ok g\u00fc\u00e7l\u00fc \u00e7ekim alan\u0131 olan ve her t\u00fcrl\u00fc maddesel olu\u015fumun ve \u0131\u015f\u0131n\u0131m\u0131n kendisinden ka\u00e7mas\u0131na izin vermeyecek derecede g\u00fc\u00e7l\u00fc olan, k\u00fctlesi b\u00fcy\u00fck bir kozmik cisim<\/p>\n<p><img fetchpriority=\"high\" decoding=\"async\" class=\"size-full wp-image-13595 aligncenter\" src=\"https:\/\/hayrettinkagnici.com\/wp-content\/uploads\/S\u00fcpernova-Nedir-1.jpg\" alt=\"\" width=\"753\" height=\"454\" srcset=\"https:\/\/hayrettinkagnici.com\/wp-content\/uploads\/S\u00fcpernova-Nedir-1.jpg 753w, https:\/\/hayrettinkagnici.com\/wp-content\/uploads\/S\u00fcpernova-Nedir-1-300x181.jpg 300w, https:\/\/hayrettinkagnici.com\/wp-content\/uploads\/S\u00fcpernova-Nedir-1-700x422.jpg 700w, https:\/\/hayrettinkagnici.com\/wp-content\/uploads\/S\u00fcpernova-Nedir-1-200x121.jpg 200w\" sizes=\"(max-width: 753px) 100vw, 753px\" \/><\/p>\n<p>veya<\/p>\n<p>uzay da belirli nicelikteki maddenin bir noktaya toplanmas\u0131 ile meydana gelen bir nesnedir. Bu t\u00fcr nesneler \u0131\u015f\u0131k yaymad\u0131klar\u0131ndan kara olarak nitelendirilirler. Kara deliklerin, \u201ctekillik\u201dleri dolay\u0131s\u0131yla, \u00fc\u00e7 boyutlu olmad\u0131klar\u0131, s\u0131f\u0131r hacimli olduklar\u0131 kabul edilir ve i\u00e7inde zaman\u0131n yava\u015f akt\u0131\u011f\u0131 veya akmad\u0131\u011f\u0131 tahmin edilmektedir. Do\u011frudan g\u00f6zlemlenememekle birlikte, \u00e7e\u015fitli dalga boylar\u0131n\u0131 kullanan g\u00f6zlem teknikleri sayesinde ke\u015ffedilmi\u015flerdir. Bu teknikler ayn\u0131 zamanda \u00e7evrelerinde s\u00fcr\u00fcklenen bir\u00e7ok olu\u015fumlar\u0131n da incelenme olana\u011f\u0131n\u0131 sa\u011flam\u0131\u015ft\u0131r. \u00d6rne\u011fin, bir kara deli\u011fin potansiyel kuyusunun \u00e7ok derin olmas\u0131 nedeniyle yak\u0131n \u00e7evresinde olu\u015facak y\u0131\u011f\u0131lma, diskinin \u00fczerine d\u00fc\u015fen maddeler nedeniyle diskin \u00e7ok y\u00fcksek s\u0131cakl\u0131klara eri\u015fmesine neden olacak, bu da diskten yani kara delikten yay\u0131lan x-\u0131\u015f\u0131nlar\u0131n\u0131n yay\u0131lmas\u0131na yol a\u00e7acakt\u0131r. Bu x-\u0131\u015f\u0131nlar\u0131 sayesinde kare delikler hakk\u0131nda bilgi alabiliyoruz.<\/p>\n<p>D\u00fcnya&#8217;dan sadece 1000 \u0131\u015f\u0131k y\u0131l\u0131 uzakl\u0131kta bulunan HR 6819 ismi verilen kara delik sistemindeki iki y\u0131ld\u0131z, D\u00fcnya&#8217;dan \u00e7\u0131plak g\u00f6zle g\u00f6r\u00fclebiliyor. 2019 y\u0131l\u0131nda, g\u00fcne\u015ften 7 milyar kat daha b\u00fcy\u00fck k\u00fctleye sahip eliptik galaksi Messier 87&#8217;nin merkezindeki s\u00fcper k\u00fctleli bir kara delik daha ke\u015ffedilmi\u015ftir. Ufku sadece 75 kilometre geni\u015fli\u011finde olmas\u0131na ra\u011fmen 10 g\u00fcne\u015f k\u00fctlesine sahip, d\u00f6nmeyen bir kara deli\u011fin yaratt\u0131\u011f\u0131 ivmelenme, d\u00fcnya y\u00fczeyindekinin yakla\u015f\u0131k 400 milyon kat\u0131d\u0131r.<\/p>\n<p>Bir karadeli\u011fin arkas\u0131nda bulunan bir y\u0131ld\u0131zdan \u00e7\u0131kan \u0131\u015f\u0131k \u0131\u015f\u0131n\u0131 bize, kara deli\u011fin \u00e7ekimsel etkisiyle ikiye ayr\u0131l\u0131r dolay\u0131s\u0131yla o y\u0131ld\u0131z\u0131 \u00e7iftmi\u015f gibi g\u00f6r\u00fcn\u00fcr. Kara delik veya bir ba\u015fka galaksi gibi \u00e7ekim kaynaklar\u0131nca \u0131\u015f\u0131k \u0131\u015f\u0131nlar\u0131na yap\u0131lan bu t\u00fcr \u00e7ekimsel m\u00fcdahale olaylar\u0131na ve zahiri sonu\u00e7lar\u0131na &#8220;\u00e7ekimsel mercek&#8221; etkisi denir.<\/p>\n<p><strong><em>Beyaz delik;<\/em><\/strong><\/p>\n<p>Beyaz delik, kara deli\u011fe d\u00fc\u015fen bir maddenin solucan delikleri arac\u0131l\u0131\u011f\u0131yla evrenin ba\u015fka bir yerinde yeniden ortaya \u00e7\u0131kt\u0131\u011f\u0131 noktalard\u0131r. Ba\u015fka bir zamana veya ba\u015fka bir \u201cbebek evren\u201d e de a\u00e7\u0131labilirler. Kara delikler, i\u00e7ine d\u00fc\u015fen hi\u00e7bir \u015feyin (\u0131\u015f\u0131k dahil) kendisinden ka\u00e7amad\u0131\u011f\u0131 cisimlerdir. Kara delik, enerjisi biten ve bu t\u00fckenme sonucu kendi i\u00e7ine do\u011fru \u00e7\u00f6kmeye ba\u015flayan y\u0131ld\u0131zlar\u0131n \u00e7ok b\u00fcy\u00fck seviyede \u00e7\u00f6kmeler ya\u015famas\u0131yla olu\u015fur. Beyaz deliklere ise hi\u00e7bir madde giremez ve bu sebeple beyaz delik olarak adland\u0131r\u0131lm\u0131\u015flard\u0131r.<\/p>\n<p><strong><em>S\u00fcpernova, <\/em><\/strong><\/p>\n<p>Enerjisi biten b\u00fcy\u00fck y\u0131ld\u0131zlar\u0131n \u015fiddetle patlamas\u0131 durumuna verilen add\u0131r. Patlama sonucunda da\u011f\u0131lan y\u0131ld\u0131z art\u0131klar\u0131n\u0131n, evrenin ba\u015fka k\u00f6\u015felerinde birikerek yeniden y\u0131ld\u0131zlar ya da y\u0131ld\u0131z sistemleri olu\u015fturdu\u011fu<img decoding=\"async\" class=\"alignright wp-image-13592\" src=\"https:\/\/hayrettinkagnici.com\/wp-content\/uploads\/Ads\u0131z-150x150.png\" alt=\"\" width=\"279\" height=\"300\" \/> varsay\u0131lmaktad\u0131r.G\u00fcne\u015f, G\u00fcne\u015f Sistemi i\u00e7indeki gezegenler ve bizim d\u00fcnyam\u0131z da, \u00e7ok eski zamanlarda ger\u00e7ekle\u015fmi\u015f bir s\u00fcpernova patlamas\u0131n\u0131n sonucunda ortaya \u00e7\u0131km\u0131\u015ft\u0131r.<\/p>\n<p><strong><em>Polaris, kuzey kutup y\u0131ld\u0131z\u0131;<\/em><\/strong><\/p>\n<p>Kutup Y\u0131ld\u0131z\u0131 ya da bilimsel ad\u0131yla Polaris, K\u00fc\u00e7\u00fck ay\u0131 tak\u0131my\u0131ld\u0131z\u0131n\u0131n en parlak y\u0131ld\u0131z\u0131 olup d\u00fcnyan\u0131n ekseni ile hemen hemen ayn\u0131 do\u011frultuda oldu\u011fundan, di\u011fer g\u00f6kcisimlerinin aksine g\u00fcn boyunca yer de\u011fi\u015ftirmez ve hep kuzeyi g\u00f6sterir. \u00a0Bu \u00f6zelli\u011fi nedeniyle tarih boyunca y\u00f6n bulma ve seyir amac\u0131yla kullan\u0131lm\u0131\u015f ve Demirkaz\u0131k, \u015eimal y\u0131ld\u0131z\u0131, Kuzey Y\u0131ld\u0131z\u0131 gibi isimler alm\u0131\u015ft\u0131r.<\/p>\n<p>Polaris, 23,5<sup>0<\/sup> derece dikeyle ka\u00e7\u0131k olarak kendi ekseni etraf\u0131nda d\u00f6nen d\u00fcnyan\u0131n ekseni ilet am olarak ayn\u0131 do\u011frultuda de\u011fildir, aradaki fark sadece bir derecenin d\u00f6rtte \u00fc\u00e7\u00fc yani 44\u2019 dakika kadard\u0131r. D\u00fcnyan\u0131n ekseni zamanla do\u011frultu de\u011fi\u015ftirdi\u011finden bu fark \u00f6n\u00fcm\u00fczdeki iki y\u00fczy\u0131l boyunca daha da azalacak ve 25\u2019 dakikaya kadar d\u00fc\u015fecek, daha sonra Kutup Y\u0131ld\u0131z\u0131 d\u00fcnyan\u0131n ekseninden giderek uzakla\u015facak ve ancak 25.000 y\u0131l sonra ayn\u0131 yere d\u00f6necektir. Bakal\u0131m d\u00f6necek mi? \u00f6mr\u00fcm\u00fcz yeterse g\u00f6rece\u011fiz,<\/p>\n<p>Kutup Y\u0131ld\u0131z\u0131, asl\u0131nda \u00fc\u00e7 y\u0131ld\u0131zdan olu\u015fan bir sistemdir. Sistemin en parlak y\u0131ld\u0131z\u0131 olan A; b\u00fcy\u00fck sar\u0131 renkli ve parlakl\u0131\u011f\u0131 en fazla oland\u0131r. Bunun \u00e7evresinde d\u00f6nen ve bir sar\u0131 c\u00fcce olan B y\u0131ld\u0131z\u0131, 1780&#8217;de William Herschel taraf\u0131ndan ke\u015ffedilmi\u015ftir. \u00dc\u00e7\u00fcnc\u00fc c\u00fcce y\u0131ld\u0131z\u0131n varl\u0131\u011f\u0131 1929&#8217;da saptanm\u0131\u015ft\u0131r. G\u00fcne\u015f&#8217;ten yakla\u015f\u0131k 2450 kere daha b\u00fcy\u00fckt\u00fcr. Di\u011fer y\u0131ld\u0131zlara g\u00f6re rengi Sar\u0131ya d\u00f6n\u00fckt\u00fcr.<\/p>\n<p>Kutup Y\u0131ld\u0131z\u0131&#8217;n\u0131 g\u00f6ky\u00fcz\u00fcnde bulmak olduk\u00e7a kolayd\u0131r, daima pusulan\u0131n kuzey ibresi do\u011frultusunda bulunur. B\u00fcy\u00fckay\u0131 tak\u0131my\u0131ld\u0131z\u0131n\u0131n olu\u015fturdu\u011fu tavan\u0131n g\u00f6vdesinin sonundaki iki parlak y\u0131ld\u0131z olan Dabne ve Merak y\u0131ld\u0131zlar\u0131n\u0131n devam\u0131 do\u011frultusunda, bu iki y\u0131ld\u0131z aras\u0131ndaki mesafenin 5 kat uzakl\u0131\u011f\u0131nda bulunur. \u00a0G\u00f6ky\u00fcz\u00fcn\u00fcn bu b\u00f6lgesindeki en parlak y\u0131ld\u0131z oldu\u011fundan, ba\u015fka bir y\u0131ld\u0131zla kar\u0131\u015ft\u0131r\u0131lma ihtimali d\u00fc\u015f\u00fckt\u00fcr. Kutup Y\u0131ld\u0131z\u0131n\u0131n ufuktan y\u00fcksekli\u011fi, bulundu\u011funuz enlemi yans\u0131tacakt\u0131r. \u00d6rne\u011fin, \u0130stanbul&#8217;da Kutup Y\u0131ld\u0131z\u0131 ufuktan 41\u00b0 y\u00fckseklikte g\u00f6r\u00fcn\u00fcr.<\/p>\n<p>Kutup Y\u0131ld\u0131z\u0131, ad\u0131ndan da belli olaca\u011f\u0131 gibi sadece kuzey yar\u0131k\u00fcreden g\u00f6r\u00fcn\u00fcr, g\u00fcney yar\u0131k\u00fcreden g\u00f6r\u00fcnmez, g\u00fcneyi g\u00f6steren parlak bir g\u00fcney Kutup Y\u0131ld\u0131z\u0131 bulunmamaktad\u0131r. Ancak g\u00fcney ha\u00e7\u0131 tak\u0131my\u0131ld\u0131z\u0131, g\u00fcney yar\u0131k\u00fcrede bulunanlara kabaca g\u00fcney y\u00f6n\u00fcn\u00fc g\u00f6sterir.<\/p>\n<p><strong><em>Astro foto\u011fraf\u00e7\u0131l\u0131k;<\/em><\/strong><\/p>\n<p>Foto\u011frafa merak\u0131n\u0131z var ve de y\u0131ld\u0131z foto\u011fraflar\u0131na da ilgi duyuyorsan\u0131z, gece \u00e7ekim teknikleri d\u0131\u015f\u0131nda astromi ve y\u0131ld\u0131zlar hakk\u0131nda baz\u0131 konular\u0131 da bilmeniz gerekir. Y\u0131ld\u0131z d\u00f6ng\u00fc foto\u011fraf\u0131 \u00e7ekmek istedi\u011finizde, polaris, kuzey kutup y\u0131ld\u0131z\u0131n tam olarak berede oldu\u011funu tespit edip kadraj\u0131 ona g\u00f6re ayarlaman\u0131z gerekir Saman yolu g\u00f6k ada y\u0131ld\u0131z k\u00fcmesinin de nerede ne zaman ve ne \u015fartlarda g\u00f6z\u00fckebildi\u011fi bilirsek \u00e7ekebiliriz.<\/p>\n<p>&nbsp;<\/p>\n<p>Sevgilerimle<\/p>\n<p>Hayrettin Ka\u011fn\u0131c\u0131<\/p>\n<p>Eyl\u00fcl 2020<\/p>\n<p>&nbsp;<\/p>\n<p>&nbsp;<\/p>\n<p>&nbsp;<\/p>\n<p>&nbsp;<\/p>\n<p>&nbsp;<\/p>","protected":false},"excerpt":{"rendered":"<p>&nbsp; Cosmos, i\u00e7inde d\u00fcnyam\u0131z ve g\u00fcne\u015f sistemi olan Samanyolu galaksisi gibi 2 trilyon ba\u015fka galaksilerin ayr\u0131ca uzay dedi\u011fimiz b\u00fcy\u00fck bo\u015fluklar\u0131, rakamlara s\u0131\u011fmayacak kadar \u00e7ok y\u0131ld\u0131z ve gezegenlerin oldu\u011fu devasa boyutta bir yerdir. Samanyolu galaksisi bile \u015fu anda 2500 gezegenin isimlendirilerek takip edildi\u011fi ancak toplam 3,2 milyon gezegen ve 50 milyar y\u0131ld\u0131z\u0131n oldu\u011fu bir alan. Havan\u0131n [&hellip;]<\/p>\n","protected":false},"author":2,"featured_media":13428,"comment_status":"closed","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"footnotes":""},"categories":[13],"tags":[],"class_list":["post-13435","post","type-post","status-publish","format-standard","has-post-thumbnail","hentry","category-gezi-notlari"],"yoast_head":"<!-- This site is optimized with the Yoast SEO plugin v24.8.1 - https:\/\/yoast.com\/wordpress\/plugins\/seo\/ -->\n<title>Samanyolu Galaksisi ve Cosmos - Hayrettin Ka\u011fn\u0131c\u0131 Resmi Web Sitesi<\/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:\/\/hayrettinkagnici.com\/tr\/?p=13435\" \/>\n<meta property=\"og:locale\" content=\"tr_TR\" \/>\n<meta property=\"og:type\" content=\"article\" \/>\n<meta property=\"og:title\" content=\"Samanyolu Galaksisi ve Cosmos - Hayrettin Ka\u011fn\u0131c\u0131 Resmi Web Sitesi\" \/>\n<meta property=\"og:description\" content=\"&nbsp; Cosmos, i\u00e7inde d\u00fcnyam\u0131z ve g\u00fcne\u015f sistemi olan Samanyolu galaksisi gibi 2 trilyon ba\u015fka galaksilerin ayr\u0131ca uzay dedi\u011fimiz b\u00fcy\u00fck bo\u015fluklar\u0131, rakamlara s\u0131\u011fmayacak kadar \u00e7ok y\u0131ld\u0131z ve gezegenlerin oldu\u011fu devasa boyutta bir yerdir. Samanyolu galaksisi bile \u015fu anda 2500 gezegenin isimlendirilerek takip edildi\u011fi ancak toplam 3,2 milyon gezegen ve 50 milyar y\u0131ld\u0131z\u0131n oldu\u011fu bir alan. 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