NASA Hubble Uzay Teleskobu resmi hesab\u0131ndan payla\u015f\u0131lan videoda D\u00fcnya\u2019dan tam 655 \u0131\u015f\u0131k y\u0131l\u0131 uzakl\u0131kta bulunan Helix Nebulas\u0131\u2019n\u0131n g\u00f6r\u00fcnt\u00fcs\u00fcn\u00fcn sese d\u00f6n\u00fc\u015ft\u00fcr\u00fclm\u00fc\u015f halini payla\u015ft\u0131.<\/p>\n
G\u00f6r\u00fcnt\u00fcy\u00fc taray\u0131p renklerine g\u00f6re sese d\u00f6n\u00fc\u015ft\u00fcr\u00fclerek ortaya \u00e7\u0131kar\u0131lan videoda k\u0131rm\u0131z\u0131 \u0131\u015f\u0131k daha du\u0308s\u0327u\u0308k, mavi \u0131\u015f\u0131k ise daha y\u00fcksek at\u0131\u015flara g\u00f6re haritaland\u0131r\u0131ld\u0131. I\u015f\u0131\u011f\u0131n frekanslar\u0131n\u0131n k\u0131rm\u0131z\u0131dan maviye do\u011fru y\u00fckseldik\u00e7e, sesin frekans\u0131 da o do\u011frultuda artt\u0131\u011f\u0131 videoda ortaya \u00e7\u0131kan videoda herkesi \u015fa\u015fk\u0131nl\u0131\u011fa u\u011fratan ve \u00fcrpertici bir ses ortaya \u00e7\u0131kt\u0131.<\/p>\n
HELIX NEBULASI (HELIS BULUTSUSU)<\/b><\/p>\n
Helis Bulutsusu (di\u011fer adlar\u0131yla Helix Bulutsusu, NGC 7293 veya Caldwell 63), Kova tak\u0131my\u0131ld\u0131z\u0131 y\u00f6n\u00fcnde bulunan olduk\u00e7a b\u00fcy\u00fck bir gezegenimsi bulutsu. Karl Ludwig Harding taraf\u0131ndan muhtemelen 1824’ten \u00f6nce ke\u015ffedilmi\u015ftir. Bu bulutsu, parlak gezegenimsi bulutsular i\u00e7inde D\u00fcnya’ya en yak\u0131n olan\u0131d\u0131r. Uzakl\u0131\u011f\u0131 yakla\u015f\u0131k olarak 215 parsek yani 700 \u0131\u015f\u0131k y\u0131l\u0131d\u0131r. G\u00f6r\u00fcn\u00fc\u015fte Halka bulutsusu’na, boyutu, ya\u015f\u0131 ve fiziksel \u00f6zellikleri nedeniyle de Halter bulutsusu’na benzemektedir. Helis, 2003’ten bu yana internette s\u0131kl\u0131kla “Tanr\u0131’n\u0131n g\u00f6z\u00fc” olarak an\u0131l\u0131r. \u00dcnl\u00fc TV dizisi Battlestar Galactica’n\u0131n 15 Aral\u0131k 2006 tarihinde yay\u0131nlanan The Eye of Jupiter b\u00f6l\u00fcm\u00fcnde Helis bulutsusuna muhtemelen bir g\u00f6nderme vard\u0131r.<\/p>\n
Helis Bulutsusu, bir y\u0131ld\u0131z\u0131n evriminin son a\u015famas\u0131ndaki ‘gezegenimsi’ olu\u015fumun tipik bir \u00f6rne\u011fidir. Y\u0131ld\u0131z\u0131n \u00e7evresindeki gazlar bizim bulundu\u011fumuz noktadan alttaki bir helezon yap\u0131s\u0131na bak\u0131yormu\u015fuz gibi g\u00f6r\u00fcn\u00fcr. Bulutsunun merkezindeki y\u0131ld\u0131z, 30.000 y\u0131l \u00f6nce d\u0131\u015f katmanlar\u0131n\u0131 uzaya salm\u0131\u015f olan \u00e7ok s\u0131cak (110.000 derece) bir beyaz c\u00fccedir. Merkezi y\u0131ld\u0131zda g\u00f6zlenen k\u0131rm\u0131z\u0131l\u0131\u011f\u0131 \u00f6ylesine enerjiktir ki \u00e7evresindeki gazlar\u0131 bir floresans gibi ayd\u0131nlat\u0131r. Helis Bulutsusu’nun i\u00e7 kenarlar\u0131ndan al\u0131nan yak\u0131n \u00e7ekim g\u00f6r\u00fcnt\u00fcler, k\u00f6keni hen\u00fcz bilinmeyen karma\u015f\u0131k gaz d\u00fc\u011f\u00fcmlerini g\u00f6zler \u00f6n\u00fcne sermektedir.<\/p>\n
NASA’n\u0131n Spitzer K\u0131z\u0131l\u00f6tesi Teleskobu, bulutsu’nun merkezinde, olas\u0131 kuyrukluy\u0131ld\u0131z \u00e7ekirdekleri gibi kat\u0131 cisimlerin \u00e7arp\u0131\u015fmas\u0131ndan olu\u015fan tozlu bir disk belirlemi\u015ftir. Merkezdeki y\u0131ld\u0131z\u0131n uzaya p\u00fcsk\u00fcren d\u0131\u015f katmanlar\u0131n\u0131n \u00e7evredeki tozu s\u00fcp\u00fcrm\u00fc\u015f olmas\u0131 gerekirdi. Ancak Spitzer teleskopu, y\u0131ld\u0131zdan 35-150 Astronomik birim uzakl\u0131kta bir disk olu\u015fturan yo\u011fun tozun varl\u0131\u011f\u0131n\u0131 belirlemi\u015ftir (Soldaki resmin merkezindeki k\u0131rm\u0131z\u0131 daire, \u00e7ok k\u00fc\u00e7\u00fck oldu\u011fu i\u00e7in net g\u00f6r\u00fcnt\u00fclenemeyen diskin olu\u015fturdu\u011fu parlama). Astronomlar bu tozun, bizim G\u00fcne\u015f Sistemimizin d\u0131\u015f s\u0131n\u0131rlar\u0131ndaki Kuiper ku\u015fa\u011f\u0131’ndakiler gibi kat\u0131 cisimlerin \u00e7arp\u0131\u015fmas\u0131n\u0131n kal\u0131nt\u0131s\u0131 oldu\u011fu g\u00f6r\u00fc\u015f\u00fcndeler. E\u011fer \u015fimdi beyaz c\u00fcce olan orijinal y\u0131ld\u0131z\u0131n \u00e7evresinde bir zamanlar b\u00fcy\u00fck k\u00fctleli gezegenler dola\u015f\u0131yorduysa, y\u0131ld\u0131z\u0131n d\u0131\u015f katmanlar\u0131n\u0131 uzaya salarak k\u00fctle kaybetmesi nedeniyle y\u00f6r\u00fcngelerinin karma\u015faya kap\u0131lmas\u0131, bunun da Helis’deki Kuiper Ku\u015fa\u011f\u0131 benzerini kar\u0131\u015ft\u0131rm\u0131\u015f olmas\u0131 ve nisb\u00ee \u00e7ok say\u0131da \u00e7arp\u0131\u015fmaya yol a\u00e7m\u0131\u015f olmas\u0131 olas\u0131l\u0131k olarak d\u00fc\u015f\u00fcn\u00fclmektedir. Ayr\u0131ca, hareketlendirilen enkaz\u0131n bir k\u0131sm\u0131n\u0131n beyaz c\u00fcce \u00fczerine d\u00fc\u015fm\u00fc\u015f olmas\u0131 gerekir. Bu da \u015fimdiye kadar tam anla\u015f\u0131lamayan bir olguya; beyaz c\u00fccenin yayd\u0131\u011f\u0131 ola\u011fand\u0131\u015f\u0131 \u00f6l\u00e7ekte X-\u0131\u015f\u0131nlar\u0131na bir a\u00e7\u0131klama getirmektedir.<\/p>\n