{"id":3805,"date":"2010-01-08T03:30:36","date_gmt":"2010-01-08T00:30:36","guid":{"rendered":"http:\/\/localhost\/wordpress\/2010\/01\/08\/gunes-sistemi\/"},"modified":"2010-01-08T03:30:36","modified_gmt":"2010-01-08T00:30:36","slug":"gunes-sistemi","status":"publish","type":"post","link":"https:\/\/narteks.net\/index.php\/2010\/01\/08\/gunes-sistemi\/","title":{"rendered":"G\u00fcne\u015f Sistemi"},"content":{"rendered":"

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G\u00fcne\u015f, g\u00fcne\u015f sisteminin merkezinde yer alan y\u0131ld\u0131zd\u0131r. Yakla\u015f\u0131k 1,4 milyon km. \u00e7apl\u0131 sar\u0131 bir ana kol y\u0131ld\u0131zd\u0131r. yer Samanyolu g\u00f6kadas\u0131nda bilinen 200 milyar y\u0131ld\u0131zdan birisi olan G\u00fcne\u015f , k\u00fctlesi s\u0131cak gazlardan olu\u015fan ve \u00e7evresine \u0131s\u0131 ve \u0131\u015f\u0131k yayan bir y\u0131ld\u0131zd\u0131r . Orta b\u00fcy\u00fckl\u00fckte olan G\u00fcne\u015f tek ba\u015f\u0131na G\u00fcne\u015f Sistemi’nin k\u00fctlesinin % 99,8’ini olu\u015fturur. Geri kalan k\u00fctle G\u00fcne\u015f’in \u00e7evresinde d\u00f6nen gezegenler, asteroitler, g\u00f6kta\u015flar\u0131, kuyrukluy\u0131ld\u0131zlar ve kozmik tozdan olu\u015fur. G\u00fcn\u0131\u015f\u0131\u011f\u0131 \u015feklinde G\u00fcne\u015f’ten yay\u0131lan enerji, fotosentez yoluyla D\u00fcnya \u00fczerisindeki hayat\u0131n hemen hemen tamam\u0131n\u0131n varolmas\u0131n\u0131 sa\u011flar ve D\u00fcnya’n\u0131n iklimiyle hava durumunun \u00fczerinde \u00f6nemli etkilerde bulunur.G\u00fcne\u015fin \u00e7ap\u0131 d\u00fcnya \u00e7ap\u0131n\u0131n 109 kat\u0131 (1.5 milyon km), hacmi 1.3 milyon kat\u0131 ve a\u011f\u0131rl\u0131\u011f\u0131 333.000 kat\u0131 kadard\u0131r. G\u00fcne\u015fin yo\u011funlu\u011fu ise D\u00fcnyan\u0131n yo\u011funlu\u011funun \u00bc\u2019\u00fc kadard\u0131r. G\u00fcne\u015f kendi ekseni etraf\u0131nda saatte 70 000 km h\u0131zla d\u00f6ner. Bir turunu ise 25 g\u00fcnde tamamlar.<\/p>\n

G\u00fcne\u015f % 70hidrojen, helyum ve %5 de di\u011fer elementlerden olu\u015fur. G\u00fcne\u015fte hidrojenin helyuma d\u00f6n\u00fc\u015fmesi s\u0131ras\u0131nda (f\u00fczyon – erime birle\u015fme) b\u00fcy\u00fck bir enerji ortaya \u00e7\u0131kar. Saniyede 600 milyon ton hidrojen helyuma d\u00f6n\u00fc\u015f\u00fcr. Buda her saniye G\u00fcne\u015f`in 4.5 milyon ton hafiflemesine yol a\u00e7ar. G\u00fcne\u015fteki f\u00fczyon olay\u0131 sonucunda k\u0131z\u0131l k\u0131rm\u0131z\u0131ms\u0131 bir alev 15-20 bin km y\u00fckselir ki bu olaya G\u00fcne\u015f F\u0131rt\u0131nas\u0131 da denir.<\/p>\n

G\u00fcne\u015fin y\u00fczey s\u0131cakl\u0131\u011f\u0131 5500\u00b0C ve \u00e7ekirde\u011finin s\u0131cakl\u0131\u011f\u0131ysa 15,6 milyon\u00b0C\u2019dir. G\u00fcne\u015ften \u00e7\u0131kan enerjinin 2 milyonda birlik k\u0131sm\u0131 yery\u00fcz\u00fcne ula\u015f\u0131r. G\u00fcne\u015f\u2019in \u00fc\u00e7 g\u00fcnde yaym\u0131\u015f oldu\u011fu enerji, d\u00fcnyada ki t\u00fcm petrol, a\u011fa\u00e7, do\u011falgaz, vb. yak\u0131ta e\u015fde\u011ferdir. G\u00fcne\u015f \u0131\u015f\u0131nlar\u0131 8.44 dakikada yery\u00fcz\u00fcne ula\u015f\u0131r. G\u00fcne\u015f D\u00fcnyaya en yak\u0131n y\u0131ld\u0131zd\u0131r. \u00c7ekim kuvveti d\u00fcnya yer \u00e7ekiminin 28 kat\u0131d\u0131r. G\u00fcne\u015f D\u00fcnya’n\u0131n en az 1 milyon kat\u0131d\u0131r.<\/p>\n

Tayf\u0131 i\u00e7inde iyonize ve n\u00f6tr metaller oldu\u011fu kadar \u00e7ok zay\u0131f hidrojen \u00e7izgileri de bulunur. V eki (Roma rakam\u0131yla be\u015f) \u00e7o\u011fu y\u0131ld\u0131z gibi G\u00fcne\u015f’in de ana dizi \u00fczerinde oldu\u011funu g\u00f6sterir. Enerjisini hidrojen \u00e7ekirdeklerinin f\u00fczyonla helyuma d\u00f6n\u00fc\u015fmesinden elde eder ve hidrostatik denge i\u00e7indedir, yani zaman i\u00e7inde ne geni\u015fler ne de k\u00fc\u00e7\u00fcl\u00fcr. Saniyede 600 milyon ton hidrojen, helyuma d\u00f6n\u00fc\u015f\u00fcr. Bu da, G\u00fcne\u015f`in her ge\u00e7en saniye 4,5 milyon ton hafiflemesine yol a\u00e7ar. G\u00fcne\u015fteki f\u00fczyon olay\u0131 sonucunda k\u0131z\u0131l k\u0131rm\u0131z\u0131ms\u0131 bir alev 15-20 bin km y\u00fckselir ve G\u00fcne\u015f F\u0131rt\u0131nas\u0131 meydana gelir. Galaksimizde 100 milyondan fazla G2 s\u0131n\u0131f\u0131 y\u0131ld\u0131z bulunur. G\u00fcne\u015f, galaksimiz i\u00e7inde bulunan y\u0131ld\u0131zlar\u0131n % 85%’inden daha parlakt\u0131r, bu y\u0131ld\u0131zlar\u0131n \u00e7o\u011fu k\u0131rm\u0131z\u0131 c\u00fccelerdir.<\/p>\n

G\u00fcne\u015f g\u00fcn\u00fcm\u00fczde Samanyolu’nun daha b\u00fcy\u00fck olan Kahraman tak\u0131my\u0131ld\u0131z\u0131 ve Yay tak\u0131my\u0131ld\u0131z\u0131 kollar\u0131 aras\u0131nda kalan Orion Kolu’nun i\u00e7 k\u0131sm\u0131nda, Yerel Y\u0131ld\u0131zlararas\u0131 Bulut i\u00e7inde y\u00fcksek s\u0131cakl\u0131kta da\u011f\u0131n\u0131k gaz b\u00f6lgesi olan d\u00fc\u015f\u00fck yo\u011funluklu Yerel Kabarc\u0131k i\u00e7inden ge\u00e7mektedir. D\u00fcnya’ya 17 \u0131\u015f\u0131ky\u0131l\u0131 uzakl\u0131kta yer alan en yak\u0131n 50 y\u0131ld\u0131z i\u00e7inde G\u00fcne\u015f, mutlak kadir olarak d\u00f6rd\u00fcnc\u00fc s\u0131radad\u0131r (M=4,83).<\/p>\n

G\u00fcne\u015fin Yap\u0131s\u0131<\/p>\n

G\u00fcne\u015f bir sar\u0131 c\u00fccedir. G\u00fcne\u015f Sistemi’nin toplam k\u00fctlesinin yakla\u015f\u0131k % 99’unu olu\u015fturur. G\u00fcne\u015f hemen hemen m\u00fckemmel bir k\u00fcre \u015feklindedir, bas\u0131kl\u0131\u011f\u0131 yaln\u0131zca 9 milyonda birdir, yani kutuplararas\u0131 \u00e7ap\u0131 ile ekvator \u00e7ap\u0131 aras\u0131nda bulunan fark yaln\u0131zca 10 km.’dir. G\u00fcne\u015f plazma h\u00e2lindedir ve kat\u0131 de\u011fildir; dolay\u0131s\u0131yla kendi ekseni etraf\u0131nda d\u00f6nerken kademeli olarak d\u00f6ner, yani ekvatorda kutuplarda oldu\u011fundan daha h\u0131zl\u0131 d\u00f6ner. Bu ger\u00e7ek d\u00f6n\u00fc\u015f\u00fcn periyodu ekvatorda 25 g\u00fcn, kutuplarda 35 g\u00fcnd\u00fcr. Ancak D\u00fcnya G\u00fcne\u015f’in etraf\u0131nda d\u00f6nerken g\u00f6zlem noktam\u0131z s\u00fcrekli de\u011fi\u015fti\u011fi i\u00e7in G\u00fcne\u015f’in g\u00f6r\u00fcn\u00fcr d\u00f6n\u00fc\u015f\u00fc ekvatorda yakla\u015f\u0131k 28 g\u00fcn kadard\u0131r. Bu yava\u015f d\u00f6n\u00fc\u015f\u00fcn merkezka\u00e7 etkisi G\u00fcne\u015f’in ekvatorunda y\u00fczey \u00e7ekiminden 18 milyon kat daha g\u00fc\u00e7s\u00fczd\u00fcr. Ayn\u0131 zamanda gezegenlerden kaynaklanan gelgit etkisi G\u00fcne\u015f’in \u015feklini belirgin derecede etkilemez.<\/p>\n

Kayal\u0131k gezegenlerde oldu\u011fu gibi G\u00fcne\u015f’in belirli s\u0131n\u0131rlar\u0131 yoktur. D\u0131\u015f katmanlar\u0131nda, merkezinden uzakla\u015ft\u0131k\u00e7a gaz yo\u011funlu\u011fu \u00fcstel olarak azal\u0131r. Ancak a\u015fa\u011f\u0131da a\u00e7\u0131kland\u0131\u011f\u0131 gibi G\u00fcne\u015f’in belirgin bir i\u00e7 yap\u0131s\u0131 bulunur. G\u00fcne\u015f’in yar\u0131\u00e7ap\u0131 merkezinden \u0131\u015f\u0131kyuvar\u0131n\u0131n (fotosfer) kenar\u0131na kadar \u00f6l\u00e7\u00fcl\u00fcr. Bu hemen yukar\u0131s\u0131nda gazlar\u0131n \u00f6nemli miktarda \u0131\u015f\u0131k sa\u00e7amayacak kadar \u00e7ok so\u011fuk ya da \u00e7ok ince oldu\u011fu katmand\u0131r. I\u015f\u0131k yuvar\u0131 \u00e7\u0131plak g\u00f6zle g\u00f6r\u00fclen y\u00fczeydir. G\u00fcne\u015f \u00e7ekirde\u011fi toplam hacminin y\u00fczde 10’una ama toplam k\u00fctlesinin y\u00fczde 40’\u0131na sahiptir.<\/p>\n

G\u00fcne\u015f’in i\u00e7i do\u011frudan g\u00f6zlemlenemez ve G\u00fcne\u015f elektromanyetik \u0131\u015f\u0131maya kar\u015f\u0131 opakt\u0131r. Ancak nas\u0131l sismoloji deprem taraf\u0131ndan \u00fcretilen dalgalar\u0131 kullanarak D\u00fcnya’n\u0131n i\u00e7 yap\u0131s\u0131n\u0131 ortaya \u00e7\u0131kar\u0131yorsa helyosismoloji de G\u00fcne\u015f’in i\u00e7inden ge\u00e7en bas\u0131n\u00e7 dalgalar\u0131n\u0131 kullanarak i\u00e7 yap\u0131s\u0131n\u0131 \u00f6l\u00e7meye ve g\u00f6r\u00fcnt\u00fclemeye \u00e7al\u0131\u015f\u0131r. G\u00fcne\u015f’in bilgisayar modellemesi de i\u00e7 katmanlar\u0131 ara\u015ft\u0131rmak amac\u0131yla kuramsal bir ara\u00e7 olarak kullan\u0131l\u0131r.<\/p>\n

\u00c7ekirdek<\/p>\n

G\u00fcne\u015f \u00e7ekirde\u011fi merkezden 0,2 g\u00fcne\u015f yar\u0131\u00e7ap\u0131na kadar uzan\u0131r. Yo\u011funlu\u011fu 150.000 kg\/m\u00b3 (Yery\u00fcz\u00fcnde suyun yo\u011funlu\u011funun 150 kat\u0131) civar\u0131nda, s\u0131cakl\u0131\u011f\u0131 da 13.600.000 kelvin kadard\u0131r (y\u00fczey s\u0131cakl\u0131\u011f\u0131 yakla\u015f\u0131k 5.800 kelvindir). Yak\u0131n zamandaki SOHO (Solar and Heliospheric Observatory) misyonunun getirdi\u011fi bilgiler \u00e7ekirdekte i\u015f\u0131nsal b\u00f6lgeye do\u011fru daha h\u0131zl\u0131 bir d\u00f6nme h\u0131z\u0131 oldu\u011funu belirtmektedir. G\u00fcne\u015f’in ya\u015fam\u0131n\u0131n \u00e7o\u011funda enerji, proton-proton zincirleme tepkimesi diye adland\u0131r\u0131lan a\u015famalardan olu\u015fan ve hidrojeni helyuma \u00e7eviren n\u00fckleer f\u00fczyon ile olu\u015fur. \u00c7ekirdek, f\u00fczyon ile \u00f6nemli derecede \u0131s\u0131 olu\u015fturulan tek yerdir. Y\u0131ld\u0131z\u0131n geri kalan\u0131 \u00e7ekirdekten d\u0131\u015far\u0131ya do\u011fru transfer edilen enerjiyle \u0131s\u0131n\u0131r. \u00c7ekirdekte f\u00fczyonla olu\u015fan t\u00fcm enerji arka arkaya gelen katmanlardan ge\u00e7erek g\u00fcne\u015f \u0131\u015f\u0131kyuvar\u0131na ula\u015f\u0131r ve buradan uzaya g\u00fcn\u0131\u015f\u0131\u011f\u0131 ve par\u00e7ac\u0131klar\u0131n kinetik enerjisi olarak yay\u0131l\u0131r.<\/p>\n

G\u00fcne\u015f’te serbest olarak bulunan toplam ~8.9\u00d71056<\/sup> proton (hidrojen \u00e7ekirde\u011fi) her saniye 3,4\u00d71038<\/sup> kadar\u0131 helyum \u00e7ekirde\u011fine d\u00f6n\u00fc\u015f\u00fcr, saniyede 4,26 milyon ton madde-enerji d\u00f6n\u00fc\u015f\u00fcm oran\u0131yla saniyede 383 yottawatt (3,83\u00d71026<\/sup> W) ya da 9,15\u00d71010<\/sup> megaton TNT enerji a\u00e7\u0131\u011fa \u00e7\u0131kar. Bu asl\u0131nda g\u00fcne\u015f \u00e7ekirde\u011finde 0,3 \u00b5W\/cm\u00b3 ya da 6 \u00b5W\/kg madde gibi olduk\u00e7a d\u00fc\u015f\u00fck bir enerji \u00fcretimi oran\u0131na kar\u015f\u0131l\u0131k gelir. \u00d6rne\u011fin insan v\u00fccudu yakla\u015f\u0131k olarak 1,2 W\/kg \u0131s\u0131 \u00fcretir, yani bu da G\u00fcne\u015f’in birim k\u00fctle ba\u015f\u0131na milyonlarca kat\u0131 demektir. D\u00fcnya \u00fczerinde benzer parametreler kullan\u0131larak plazma ile enerji \u00fcretilmesi tamamen mant\u0131ks\u0131z olacakt\u0131r \u00e7\u00fcnk\u00fc orta kapasitede 1 GW’l\u0131k bir f\u00fczyon g\u00fc\u00e7 santral\u0131 bir k\u00fcp mil hacminde 170 milyar tonluk plazmaya ihtiya\u00e7 duyacakt\u0131r. Dolay\u0131s\u0131yla yery\u00fcz\u00fcnde bulunan f\u00fczyon reakt\u00f6rleri, G\u00fcne\u015f’in i\u00e7indekinden \u00e7ok daha y\u00fcksek plazma s\u0131cakl\u0131klar\u0131 kullanmaktad\u0131r.<\/p>\n

N\u00fckleer f\u00fczyon h\u0131z\u0131, yo\u011funluk ve s\u0131cakl\u0131\u011fa \u00e7ok yak\u0131ndan ba\u011fl\u0131d\u0131r, dolay\u0131s\u0131yla \u00e7ekirdekteki f\u00fczyon h\u0131z\u0131 kendi kendini d\u00fczenleyen bir dengeye sahiptir. Biraz y\u00fcksek bir f\u00fczyon h\u0131z\u0131 sonucunda \u00e7ekirdek \u0131s\u0131narak d\u0131\u015f katmanlara do\u011fru hafif\u00e7e geni\u015fleyecek, f\u00fczyon h\u0131z\u0131n\u0131 azaltacak ve kendini d\u00fczenleyecektir. Biraz d\u00fc\u015f\u00fck bir f\u00fczyon h\u0131z\u0131 da \u00e7ekirde\u011fin so\u011fumas\u0131na ve daralmas\u0131na dolay\u0131syla da f\u00fczyon h\u0131z\u0131n\u0131n artmas\u0131na neden olacakt\u0131r.<\/p>\n

N\u00fckleer f\u00fczyon tepkimeleri sonucunda a\u00e7\u0131\u011fa \u00e7\u0131kan y\u00fcksek enerjili fotonlar (kozmik, gama ve X \u0131\u015f\u0131nlar\u0131) g\u00fcne\u015f plazmas\u0131n\u0131n yaln\u0131zca birka\u00e7 milimetresi taraf\u0131nda emilir ve tekrar rastgele y\u00f6nlerde \u00e7ok az enerji kaybederek tekrar yay\u0131l\u0131r, bu nedenle de \u0131\u015f\u0131man\u0131n G\u00fcne\u015f’in y\u00fczeyine ula\u015fmas\u0131 uzun zaman al\u0131r. “Foton yolculuk zaman\u0131” 10.000 il\u00e2 170.000 y\u0131l kadar s\u00fcrer.<\/p>\n

Is\u0131yay\u0131msal d\u0131\u015f katmandan \u015feffaf “y\u00fczey” \u0131\u015f\u0131kyuvara do\u011fru son bir yolculuktan sonra fotonlar g\u00f6r\u00fcn\u00fcr \u0131\u015f\u0131k olarak ka\u00e7ar. G\u00fcne\u015f’in merkezinde bulunan her gama \u0131\u015f\u0131n\u0131 uzaya ka\u00e7madan \u00f6nce bir ka\u00e7 milyon g\u00f6r\u00fcn\u00fcr \u0131\u015f\u0131k fotonuna d\u00f6n\u00fc\u015f\u00fcr. N\u00f6trinolar da \u00e7ekirdekteki tepkimelerde olu\u015fur ama fotonlar\u0131n aksine nadiren madde ile etkile\u015fime girer, dolay\u0131s\u0131yla hemen hemen hepsi G\u00fcne\u015f’ten hemen ka\u00e7abilir. \u00c7ok uzun y\u0131llar, G\u00fcne\u015f’te \u00fcretilen n\u00f6trinolar\u0131n \u00f6l\u00e7\u00fcm\u00fc kuramlar sonucu tahmin edilenden 3 kat daha d\u00fc\u015f\u00fckt\u00fc. Bu tutars\u0131zl\u0131k yak\u0131n zamanda n\u00f6trino sal\u0131n\u0131m etkilerinin ke\u015ffiyle \u00e7\u00f6z\u00fcld\u00fc. G\u00fcne\u015f ger\u00e7ekten de kuramlarca \u00f6nerilen miktarda n\u00f6trinoyu a\u00e7\u0131\u011fa \u00e7\u0131karmakta ancak n\u00f6trino alg\u0131lay\u0131c\u0131lar\u0131 bunlar\u0131n \u00fc\u00e7te ikisini ka\u00e7\u0131rmaktad\u0131r \u00e7\u00fcnk\u00fc n\u00f6trinolar kuantum say\u0131lar\u0131n\u0131 de\u011fi\u015ftirmektedir.<\/p>\n

G\u00fcne\u015fin Manyetik Alan\u0131<\/p>\n

G\u00fcne\u015f i\u00e7inde bulunan t\u00fcm madde y\u00fcksek s\u0131cakl\u0131klardan \u00f6t\u00fcr\u00fc gaz ve plazma h\u00e2lindedir. Bu nedenle G\u00fcne\u015f ekvatorda yukar\u0131 enlemlerde oldu\u011fundan daha h\u0131zl\u0131 d\u00f6ner. Ekvatorda d\u00f6n\u00fc\u015f h\u0131z\u0131 25 g\u00fcn iken kutuplarda 35 g\u00fcnde kendi etraf\u0131nda d\u00f6ner. Bu kademeli d\u00f6n\u00fc\u015f sonucunda manyetik alan \u00e7izgilerinin zamanla k\u0131vr\u0131larak manyetik alan halkalar\u0131 olu\u015fturmas\u0131 G\u00fcne\u015f’in y\u00fczeyinden patlamalarla ayr\u0131larak g\u00fcne\u015f lekeleri ve g\u00fcne\u015f p\u00fcsk\u00fcrt\u00fcleri olu\u015fumuna neden olur. Bu k\u0131vr\u0131lma hareketi solar dinamonun olu\u015fmas\u0131na ve 11 y\u0131ll\u0131k G\u00fcne\u015f d\u00f6ng\u00fcs\u00fc ile G\u00fcne\u015f’in manyetik alan\u0131n\u0131n y\u00f6n de\u011fi\u015ftirmesine neden olur.<\/p>\n

G\u00fcne\u015f’in d\u00f6nen manyetik alan\u0131n\u0131n gezegenleraras\u0131 ortamda bulunan plazma \u00fczerindeki etkisi G\u00fcnyuvar ak\u0131m katman\u0131n\u0131 olu\u015fturur. Bu katman farkl\u0131 y\u00f6nleri g\u00f6steren manyetik alanlar\u0131 ay\u0131r\u0131r. Gezegenleraras\u0131 ortamda bulunan plazma ayn\u0131 zamanda D\u00fcnya’n\u0131n y\u00f6r\u00fcngesinde G\u00fcne\u015f’in manyetik alan\u0131n\u0131n kuvvetinden de sorumludur. E\u011fer uzay bir vakum olsayd\u0131 G\u00fcne\u015f’in 10-4<\/sup> tesla manyetik dipol alan\u0131 uzakl\u0131\u011f\u0131n k\u00fcb\u00fcyle azalarak 10-11<\/sup> tesla olacakt\u0131. Ancak uydu g\u00f6zlemleri bunun 100 kat daha fazla kuvvetli oldu\u011funu ve 10-9<\/sup> tesla civar\u0131nda oldu\u011funu g\u00f6stermektedir. Manyetohidrodinamik (MHD) kuram manyetik alan i\u00e7indeki iletken bir ak\u0131\u015fkan\u0131n (\u00f6rne\u011fin gezegenleraras\u0131 ortam) yine manyetik alan yaratan elektrik ak\u0131mlar\u0131 ind\u00fckledi\u011fini s\u00f6yler, dolay\u0131s\u0131yla bir MHD dinamo gibi hareket eder.<\/p>\n","protected":false},"excerpt":{"rendered":"

G\u00fcne\u015f, g\u00fcne\u015f sisteminin merkezinde yer alan y\u0131ld\u0131zd\u0131r. Yakla\u015f\u0131k 1,4 milyon km. \u00e7apl\u0131 sar\u0131 bir ana kol y\u0131ld\u0131zd\u0131r. yer Samanyolu g\u00f6kadas\u0131nda bilinen 200 milyar y\u0131ld\u0131zdan birisi olan G\u00fcne\u015f , k\u00fctlesi s\u0131cak gazlardan olu\u015fan ve \u00e7evresine \u0131s\u0131 ve \u0131\u015f\u0131k yayan bir y\u0131ld\u0131zd\u0131r . Orta b\u00fcy\u00fckl\u00fckte olan G\u00fcne\u015f tek ba\u015f\u0131na G\u00fcne\u015f Sistemi’nin k\u00fctlesinin % 99,8’ini olu\u015fturur. Geri kalan […]<\/p>\n","protected":false},"author":1,"featured_media":0,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"footnotes":""},"categories":[50],"tags":[],"class_list":{"0":"post-3805","1":"post","2":"type-post","3":"status-publish","4":"format-standard","6":"category-astronomi"},"yoast_head":"\nG\u00fcne\u015f Sistemi - narteks.net<\/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:\/\/narteks.net\/index.php\/2010\/01\/08\/gunes-sistemi\/\" \/>\n<meta property=\"og:locale\" content=\"tr_TR\" \/>\n<meta property=\"og:type\" content=\"article\" \/>\n<meta property=\"og:title\" content=\"G\u00fcne\u015f Sistemi\" \/>\n<meta property=\"og:description\" content=\"G\u00fcne\u015f, g\u00fcne\u015f sisteminin merkezinde yer alan y\u0131ld\u0131zd\u0131r. Yakla\u015f\u0131k 1,4 milyon km. \u00e7apl\u0131 sar\u0131 bir ana kol y\u0131ld\u0131zd\u0131r. yer Samanyolu g\u00f6kadas\u0131nda bilinen 200 milyar y\u0131ld\u0131zdan birisi olan G\u00fcne\u015f , k\u00fctlesi s\u0131cak gazlardan olu\u015fan ve \u00e7evresine \u0131s\u0131 ve \u0131\u015f\u0131k yayan bir y\u0131ld\u0131zd\u0131r . Orta b\u00fcy\u00fckl\u00fckte olan G\u00fcne\u015f tek ba\u015f\u0131na G\u00fcne\u015f Sistemi’nin k\u00fctlesinin % 99,8’ini olu\u015fturur. 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Yakla\u015f\u0131k 1,4 milyon km. \u00e7apl\u0131 sar\u0131 bir ana kol y\u0131ld\u0131zd\u0131r. yer Samanyolu g\u00f6kadas\u0131nda bilinen 200 milyar y\u0131ld\u0131zdan birisi olan G\u00fcne\u015f , k\u00fctlesi s\u0131cak gazlardan olu\u015fan ve \u00e7evresine \u0131s\u0131 ve \u0131\u015f\u0131k yayan bir y\u0131ld\u0131zd\u0131r . Orta b\u00fcy\u00fckl\u00fckte olan G\u00fcne\u015f tek ba\u015f\u0131na G\u00fcne\u015f Sistemi’nin k\u00fctlesinin % 99,8’ini olu\u015fturur. 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