Ara\u015ft\u0131rmac\u0131lar bu bulgular\u0131n ayr\u0131ca evrenin geni\u015flemesinin ayd\u0131nlat\u0131lmas\u0131na yard\u0131mc\u0131 olaca\u011f\u0131n\u0131 belirttiler.<\/p>\n
S\u00fcpernova, enerjisi biten B\u00fcy\u00fck Y\u0131ld\u0131zlar\u0131n \u015fiddetle patlamas\u0131 durumuna verilen add\u0131r. Bir s\u00fcpernovan\u0131n parlakl\u0131\u011f\u0131 G\u00fcne\u015f’in parlakl\u0131\u011f\u0131n\u0131n y\u00fcz milyon kat\u0131na varabilir. Ba\u015flang\u0131\u00e7ta yap\u0131s\u0131, iyonize madde olan plazma \u015feklindeki bir s\u00fcpernovan\u0131n parlakl\u0131\u011f\u0131n\u0131 yitirmesi haftalar ya da aylar s\u00fcrebilir. Tip Ia s\u00fcpernovalar\u0131 ise, alt kataklizmik de\u011fi\u015fen y\u0131ld\u0131zlar kategorisinde olan bir beyaz c\u00fcce y\u0131ld\u0131z\u0131n, \u015fiddetli patlamas\u0131n\u0131n sonu\u00e7lar\u0131ndan olu\u015fur.<\/p>\n
Son y\u0131llarda, ara\u015ft\u0131rmac\u0131lar Tip Ia s\u00fcpernovas\u0131ndan be\u015f ila on kat daha parlak yeni bir s\u00fcpernova tipi rapor etmeye ba\u015flad\u0131lar. Ad\u0131 S\u00fcper Parlak S\u00fcpernova, bir\u00e7ok ki\u015fi bu y\u0131ld\u0131zlar hakk\u0131nda daha fazla \u015fey \u00f6\u011frenmeye \u00e7al\u0131\u015f\u0131yor. Ola\u011fand\u0131\u015f\u0131 parlakl\u0131klar\u0131, ara\u015ft\u0131rmac\u0131lar\u0131n evrenin en uzak k\u0131s\u0131mlar\u0131ndaki y\u0131ld\u0131zlar\u0131 g\u00f6zlemlemesi i\u00e7in genellikle uzun bir soluk olmalar\u0131n\u0131 sa\u011flar. Bu t\u00fcr s\u00fcpernovalar B\u00fcy\u00fck Patlamadan sonra olu\u015fturulan ilk masif y\u0131ld\u0131zlar\u0131n \u00f6zelliklerini ortaya koyabilir.<\/p>\n
Fakat s\u00fcpernovalar nadir g\u00f6r\u00fclen olaylard\u0131r ve d\u00fcnyadaki uzak y\u0131ld\u0131zlar\u0131n keskin g\u00f6r\u00fcnt\u00fclerini \u00e7ekebilen sadece bir avu\u00e7 teleskop vard\u0131r.<\/p>\n
Bir s\u00fcpernova g\u00f6zlemleme \u015fans\u0131n\u0131 en \u00fcst seviyeye \u00e7\u0131karmak i\u00e7in Kavli, evrenin Fizik ve Matematik Enstit\u00fcs\u00fc (Kavli IPMU) Profes\u00f6r\u00fc Naoki Yasuda ve Japonya Ulusal Astronomik G\u00f6zlemevi, Konan \u00dcniversitesi, Japonya Ulusal Okulu Astronomi G\u00f6zlemcisi taraf\u0131ndan y\u00fcr\u00fct\u00fclen bir ekip Bilim \u00dcniversitesi, Tokyo \u00dcniversitesi ve Kyoto \u00dcniversitesi, Subaru Teleskobu’nu kulland\u0131.<\/p>\n
Bu teleskop \u015fekil y\u0131ld\u0131z g\u00f6r\u00fcnt\u00fcleri \u00fcretme yetene\u011fine sahiptir ve tepesine tak\u0131l\u0131 870 mega piksel dijital kamera olan Hyper Suprime-Cam, tek \u00e7ekimde gece g\u00f6ky\u00fcz\u00fcn\u00fcn \u00e7ok geni\u015f bir alan\u0131n\u0131 yakalar.<\/p>\n
Ara\u015ft\u0131rmac\u0131lar alt\u0131 ay boyunca ayn\u0131 gece g\u00f6ky\u00fcz\u00fcn\u00fcn tekrar tekrar g\u00f6r\u00fcnt\u00fcs\u00fcn\u00fc alarak, s\u00f6nmeden \u00f6nce aniden daha parlak g\u00f6r\u00fcnen y\u0131ld\u0131zlar\u0131 arayarak yeni s\u00fcpernovalar\u0131 belirleyebilirler.<\/p>\n
Sonu\u00e7 olarak, ekip 5 s\u00fcper ayd\u0131nl\u0131k s\u00fcpernova ve yakla\u015f\u0131k 400 Tip Ia s\u00fcpernova tan\u0131mlad\u0131. Bu Tip Ia s\u00fcpernovalar\u0131n\u0131n elli sekizi D\u00fcnya’dan 8 milyar \u0131\u015f\u0131k y\u0131l\u0131 uza\u011f\u0131nda bulunuyordu.<\/p>\n
Hubble Uzay Teleskopu’nu kullanarak D\u00fcnya’dan 8 milyar \u0131\u015f\u0131k y\u0131l\u0131 uzakta bulunan toplam 50 s\u00fcpernovay\u0131 ke\u015ffetmek yakla\u015f\u0131k 10 y\u0131l s\u00fcrd\u00fc.<\/p>\n
Naoki Yasuda, “Subaru Teleskopu ve Hyper Suprime-Cam, ara\u015ft\u0131rmac\u0131lara zaten 3 boyutlu bir karanl\u0131k madde haritas\u0131 ve ilkel kara deliklerin g\u00f6zlemlenmesi konusunda yard\u0131mc\u0131 oldu, ancak \u015fimdi bu sonu\u00e7, bu arac\u0131n s\u00fcpernovalar\u0131 \u00e7ok uzakta bulma konusunda \u00e7ok y\u00fcksek bir kabiliyete sahip oldu\u011funu kan\u0131tlad\u0131. T\u00fcm i\u015fbirlik\u00e7ilerime harcad\u0131klar\u0131 zamanlar\u0131 ve \u00e7abalar\u0131 i\u00e7in te\u015fekk\u00fcr etmek istiyorum ve evrenin nas\u0131l bir resmini tuttu\u011fumuzu g\u00f6rmek i\u00e7in verilerimizi analiz etmeyi d\u00f6rt g\u00f6zle bekliyorum.” dedi.<\/p>\n
Ba\u015flang\u0131\u00e7ta yap\u0131s\u0131, iyonize madde olan plazma \u015feklindeki bir s\u00fcpernovan\u0131n parlakl\u0131\u011f\u0131n\u0131 yitirmesi haftalar ya da aylar s\u00fcrebilir. Bu s\u00fcre zarf\u0131nda yayd\u0131\u011f\u0131 enerji, G\u00fcne\u015f’in 10 milyar y\u0131lda yayaca\u011f\u0131 enerjiden daha fazlad\u0131r. Bu patlamalar, maddenin evrende bir noktadan ba\u015fka noktalara ta\u015f\u0131nmas\u0131 i\u015fine yarar. 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 varsay\u0131lmaktad\u0131r. Bu varsay\u0131ma g\u00f6re, G\u00fcne\u015f, G\u00fcne\u015f Sistemi i\u00e7indeki gezegenler ve bu arada elbette 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
18 Eyl\u00fcl 2006 tarihinde R Quimby ve P. Mondol taraf\u0131ndan ke\u015ffedilen SN2006 gy isimli s\u00fcpernovan\u0131n \u015fimdiye kadar g\u00f6zlemlenmi\u015f en parlak s\u00fcpernova oldu\u011fu a\u00e7\u0131kland\u0131. SN2006 gy s\u00fcpernovas\u0131n\u0131n meydana geldi\u011fi galaksi NGC 1260, bize 238 milyon \u0131\u015f\u0131k y\u0131l\u0131 uzakl\u0131kta. Yani s\u00fcpernovadan gelen \u0131\u015f\u0131\u011f\u0131n d\u00fcnyam\u0131za ula\u015fmas\u0131 238 milyon y\u0131l s\u00fcrd\u00fc.<\/p>\n
S\u00fcpernova taraf\u0131ndan f\u0131rlat\u0131lan gaz kabuk y\u0131ld\u0131zlararas\u0131 ortama ilerlerken, yeni meydana gelen a\u011f\u0131r elementleri de y\u0131ld\u0131zlararas\u0131 ortama katarak zenginle\u015ftirir; buna da s\u00fcpernova kal\u0131nt\u0131s\u0131 denir. Tarihte, g\u00f6zlenen s\u00fcpernova patlamas\u0131 ile birlikte, sadece yar\u0131m d\u00fczine s\u00fcpernova kal\u0131nt\u0131s\u0131 e\u015fle\u015ftirilmi\u015ftir. 1572’de Tycuho, 1604’te Kepler ve 1054 y\u0131l\u0131nda \u00c7inli astronomlar\u0131n g\u00f6zledi\u011fi s\u00fcpernovalar bunlara \u00f6rnektir.<\/p>\n
Cygnus tak\u0131my\u0131ld\u0131z\u0131nda bulunan, D\u00fcnyaya 2500 \u0131\u015f\u0131k y\u0131l\u0131 uzakl\u0131ktaki ve Cygnus D\u00fc\u011f\u00fcm\u00fc olarak bilinen bir s\u00fcpernova kal\u0131nt\u0131s\u0131na ait s\u00fcpernova yakla\u015f\u0131k 15 000 y\u0131l \u00f6nce patlam\u0131\u015ft\u0131r. Bug\u00fcn bile devam edegelen patlamadan kalan \u015fok dalgalar\u0131 \u00e7evresindeki y\u0131ld\u0131zlararas\u0131 ortam\u0131 hala itmektedir ve i\u00e7indeki gaz\u0131 \u0131s\u0131t\u0131p X \u0131\u015f\u0131n\u0131 yaymaya devam etmektedir.<\/p>\n
G\u00f6kbilimciler s\u00fcpernovalar\u0131 anlamak i\u00e7in onlar\u0131 tayflar\u0131nda g\u00f6r\u00fcnen farkl\u0131 kimyasal \u00f6\u011felerin \u00e7izgilerine g\u00f6re s\u0131n\u0131fland\u0131rm\u0131\u015flard\u0131r. Birinci b\u00f6l\u00fcm i\u00e7in ilk \u00f6\u011fe, \u00e7izginin var olmas\u0131 veya hidrojen nedeniyle olmamas\u0131d\u0131r. E\u011fer bir s\u00fcpernovan\u0131n tayf\u0131, (Tayf\u0131n g\u00f6rsel k\u0131sm\u0131nda Balmer dizisi olarak bilinen) hidrojenin bir \u00e7izgisini i\u00e7erirse, Tip II olarak s\u0131n\u0131fland\u0131r\u0131l\u0131r; di\u011feri ise Tip I dir. Bu tipler aras\u0131ndaki altb\u00f6l\u00fcmler, di\u011fer elementlerin ve \u0131\u015f\u0131k e\u011frisi (s\u00fcpernovan\u0131n zaman i\u00e7indeki g\u00f6r\u00fcn\u00fcr parlakl\u0131\u011f\u0131n\u0131n grafi\u011fi) \u00e7izgilerinin var olmas\u0131na g\u00f6re olu\u015fturulur.<\/p>\n","protected":false},"excerpt":{"rendered":"
Ara\u015ft\u0131rmac\u0131lar bu bulgular\u0131n ayr\u0131ca evrenin geni\u015flemesinin ayd\u0131nlat\u0131lmas\u0131na yard\u0131mc\u0131 olaca\u011f\u0131n\u0131 belirttiler. S\u00fcpernova, enerjisi biten B\u00fcy\u00fck Y\u0131ld\u0131zlar\u0131n \u015fiddetle patlamas\u0131 durumuna verilen add\u0131r. Bir s\u00fcpernovan\u0131n parlakl\u0131\u011f\u0131 G\u00fcne\u015f’in parlakl\u0131\u011f\u0131n\u0131n y\u00fcz milyon kat\u0131na varabilir. Ba\u015flang\u0131\u00e7ta yap\u0131s\u0131, iyonize madde olan plazma \u015feklindeki bir s\u00fcpernovan\u0131n parlakl\u0131\u011f\u0131n\u0131 yitirmesi haftalar ya da aylar s\u00fcrebilir. Tip Ia s\u00fcpernovalar\u0131 ise, alt kataklizmik de\u011fi\u015fen y\u0131ld\u0131zlar kategorisinde olan […]<\/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-90460","post","type-post","status-publish","format-standard","hentry","category-astronomi"],"acf":[],"yoast_head":"\n