Astronomlar, NASA\u2019n\u0131n Chandra X-\u0131\u015f\u0131n\u0131 G\u00f6zlemevi\u2019ni kullanarak ilk kez Uran\u00fcs\u2019ten yay\u0131lan X-\u0131\u015f\u0131nlar\u0131n\u0131 tespit etti. Sonu\u00e7lar, ara\u015ft\u0131rmac\u0131lar\u0131n G\u00fcne\u015f Sistemi\u2019ndeki buz devi gezegen olan Uran\u00fcs hakk\u0131nda daha fazla bilgi edinmesine katk\u0131 sa\u011flayabilir.<\/p>\n
Uran\u00fcs, G\u00fcne\u015f\u2019e en yak\u0131n yedinci gezegendir. \u00c7ap\u0131 D\u00fcnya\u2019n\u0131n d\u00f6rt kat\u0131 olan Uran\u00fcs\u2019\u00fcn etraf\u0131nda iki tak\u0131m halka bulunmaktad\u0131r. Uran\u00fcs hakk\u0131ndaki \u00e7al\u0131\u015fmalara en b\u00fcy\u00fck katk\u0131 Voyager 2 g\u00f6zlemlerinden sa\u011flanm\u0131\u015ft\u0131r. Ancak astronomlar, neredeyse tamam\u0131 hidrojen ve helyumdan olu\u015fan Uran\u00fcs hakk\u0131nda daha fazla bilgi edinmek i\u00e7in Chandra X-\u0131\u015f\u0131n\u0131 G\u00f6zlemevi ve Hubble Uzay Teleskobu\u2019ndan elde edilebilecek yeni verilere g\u00fcvenmektedir.<\/p>\n
Yeni \u00e7al\u0131\u015fmada, 2002\u2019de ve daha sonra 2017\u2019de elde edilen Chandra X-\u0131\u015f\u0131n\u0131 G\u00f6zlemevi g\u00f6zlemleri kullan\u0131ld\u0131. Yak\u0131n d\u00f6nemde analiz edilen ilk g\u00f6zlem verilerinde X-\u0131\u015f\u0131nlar\u0131 net bir bi\u00e7imde tespit edilebildi. Peki, Uran\u00fcs\u2019\u00fcn X-\u0131\u015f\u0131nlar\u0131 yaymas\u0131n\u0131n sebebi ne olabilir? Astronomlar cevab\u0131n G\u00fcne\u015f oldu\u011funu d\u00fc\u015f\u00fcnmektedir. G\u00f6kbilimciler J\u00fcpiter ve Sat\u00fcrn\u2019\u00fcn de, t\u0131pk\u0131 D\u00fcnya atmosferinin G\u00fcne\u015f \u0131\u015f\u0131\u011f\u0131n\u0131 da\u011f\u0131tt\u0131\u011f\u0131 gibi G\u00fcne\u015f\u2019ten gelen X-\u0131\u015f\u0131nlar\u0131n\u0131 yayd\u0131\u011f\u0131n\u0131 g\u00f6zlemlediler. Uran\u00fcs\u2019teki X-\u0131\u015f\u0131n\u0131 yay\u0131l\u0131m\u0131n\u0131n da G\u00fcne\u015f kaynakl\u0131 oldu\u011fu d\u00fc\u015f\u00fcn\u00fclse de, Uran\u00fcs i\u00e7in ba\u015fka bir X-\u0131\u015f\u0131n\u0131 kayna\u011f\u0131 oldu\u011funa dair ipu\u00e7lar\u0131 bulunmaktad\u0131r.<\/p>\n
Olas\u0131l\u0131klardan biri Sat\u00fcrn halkalar\u0131ndakine benzer bir bi\u00e7imde Uran\u00fcs halkalar\u0131n\u0131n da X-\u0131\u015f\u0131n\u0131 \u00fcretmesidir. Uran\u00fcs, gezegene yak\u0131n olan uzay ortam\u0131nda elektronlar ve protonlar gibi y\u00fckl\u00fc par\u00e7ac\u0131klarla \u00e7evrelenmi\u015ftir. Bu y\u00fckl\u00fc par\u00e7ac\u0131klar Uran\u00fcs\u2019\u00fcn halkalar\u0131 ile \u00e7arp\u0131\u015f\u0131rsa, halkalarda X-\u0131\u015f\u0131n\u0131 parlamalar\u0131na neden olabilirler. Olas\u0131l\u0131klardan di\u011feri ise X-\u0131\u015f\u0131nlar\u0131n\u0131n bir k\u0131sm\u0131n\u0131n Uran\u00fcs’teki auroralardan kaynaklanmas\u0131d\u0131r. D\u00fcnya\u2019da da aurora ad\u0131 verilen renkli \u0131\u015f\u0131klar\u0131 g\u00f6rebiliriz. Aurora y\u00fcksek enerjili par\u00e7ac\u0131klar atmosferle etkile\u015fime girdi\u011finde g\u00f6zlenmektedir ve x \u0131\u015f\u0131n\u0131 yaymaktad\u0131r. Auroralar D\u00fcnya\u2019ya \u00f6zg\u00fc de\u011fildir. \u00d6rne\u011fin J\u00fcpiter\u2019in ve Uran\u00fcs\u2019\u00fcn de auroralar\u0131 vard\u0131r. Ancak ara\u015ft\u0131rmac\u0131lar, J\u00fcpiter\u2019den farkl\u0131 olarak Uran\u00fcs\u2019teki auroralar\u0131n kayna\u011f\u0131 hakk\u0131nda \u00e7ok az bilgiye sahiptir. Chandra\u2019dan elde edilen veriler bu konuda yeni ke\u015fifleri beraberinde getirebilir.<\/p>\n
Uran\u00fcs\u2019\u00fcn bir ba\u015fka \u00f6zelli\u011fi, onu X-\u0131\u015f\u0131n\u0131 g\u00f6zlemleri i\u00e7in ilgin\u00e7 bir hedef haline getirmektedir. G\u00fcne\u015f Sistemi\u2019ndeki di\u011fer gezegenlerin d\u00f6n\u00fc\u015f ve manyetik alan eksenleri kendi y\u00f6r\u00fcngelerine neredeyse dik konumdad\u0131r ancak Uran\u00fcs\u2019\u00fcn d\u00f6n\u00fc\u015f ekseni G\u00fcne\u015f etraf\u0131ndaki d\u00f6n\u00fc\u015f yoluna neredeyse paralel bir konumda yer almaktad\u0131r. Ek olarak, Uran\u00fcs d\u00f6n\u00fc\u015f\u00fc s\u0131ras\u0131nda gezegenin manyetik alan\u0131 farkl\u0131 bir a\u00e7\u0131da d\u00f6n\u00fc\u015f yapar ve gezegenin merkezinden bir miktar kayar. Bu gibi ilgin\u00e7 \u00f6zellikleri nedeniyle Uran\u00fcs\u2019\u00fcn ve Uran\u00fcs\u2019ten gelen X-\u0131\u015f\u0131nlar\u0131n\u0131n kayna\u011f\u0131n\u0131n daha geni\u015f bir \u00e7er\u00e7evede anla\u015f\u0131lmas\u0131, kara delikler ve n\u00f6tron y\u0131ld\u0131zlar\u0131 gibi nesnelerin nas\u0131l X-\u0131\u015f\u0131n\u0131 yayd\u0131\u011f\u0131n\u0131 anlamaya yard\u0131mc\u0131 olabilir.<\/p>\n