Finlandiya\u2019daki Turku \u00dcniversitesinde \u00e7al\u0131\u015fan ara\u015ft\u0131rmac\u0131lar, ikili bir y\u0131ld\u0131z sisteminde yer alan bir kara deli\u011fin d\u00f6nme ekseninin, y\u0131ld\u0131z\u0131n y\u00f6r\u00fcnge eksenine g\u00f6re 40 dereceden fazla e\u011fik durdu\u011funu ke\u015ffetti. Bulgular, kara delik olu\u015fumuna d\u00f6n\u00fck mevcut kuramsal modellere meydan okuyor.<\/p>\n
Finlandiya\u2019daki Tuorla G\u00f6zlemevi’nde \u00e7al\u0131\u015fan ara\u015ft\u0131rmac\u0131lar\u0131n yeni g\u00f6zlemi, bir kara deli\u011fin d\u00f6nme ekseni ile ikili bir y\u0131ld\u0131z sisteminin y\u00f6r\u00fcnge ekseni aras\u0131nda b\u00fcy\u00fck bir farkl\u0131l\u0131k oldu\u011funu g\u00f6steren ilk g\u00fcvenilir \u00f6l\u00e7\u00fcm niteli\u011finde. Ara\u015ft\u0131rmac\u0131lar\u0131n MAXI J1820+070 adl\u0131 ikili bir y\u0131ld\u0131z sistemindeki eksenler aras\u0131nda \u00f6l\u00e7t\u00fc\u011f\u00fc bu farkl\u0131l\u0131k, 40 dereceden fazla.
\nGenel olarak merkezdeki dev bir cismin etraf\u0131nda d\u00f6nen daha k\u00fc\u00e7\u00fck cisimlerin yer ald\u0131\u011f\u0131 uzay sistemlerinde, merkez cismin d\u00f6n\u00fc\u015f ekseni, uydular\u0131n\u0131n d\u00f6n\u00fc\u015f eksenleriyle y\u00fcksek bir dereceye kadar uyum g\u00f6steriyor. Bu durum, kendi g\u00fcne\u015f sistemimizde de ge\u00e7erli: Gezegenler G\u00fcne\u015f\u2019in etraf\u0131nda, G\u00fcne\u015f\u2019in ekvatoral d\u00fczlemiyle hemen hemen denk d\u00fc\u015fen bir d\u00fczlemde d\u00f6n\u00fcyor. G\u00fcne\u015f\u2019in d\u00f6nme eksenindeki bu e\u011fri, D\u00fcnya\u2019n\u0131n y\u00f6r\u00fcnge eksenine g\u00f6re sadece yedi derece.<\/p>\n
Kara delik X \u0131\u015f\u0131n\u0131<\/span><\/h2>\n Turku \u00dcniversitesi’nde g\u00f6kbilim profes\u00f6r\u00fc ve yeni \u00e7al\u0131\u015fman\u0131n ba\u015f yazar\u0131 olan Juri Poutanen \u015f\u00f6yle aktard\u0131: \u201cHiza beklentisi, kara delik X-\u0131\u015f\u0131n\u0131 ikilileri gibi tuhaf cisimlerde \u00e7o\u011funlukla ge\u00e7erli olmuyor. Bu sistemlerdeki kara delikler, kozmik bir afetin sonucunda; dev bir y\u0131ld\u0131z\u0131n \u00e7\u00f6k\u00fc\u015f\u00fcyle olu\u015fmu\u015f. Kara deli\u011fin yak\u0131n\u0131ndan; yani etraf\u0131nda d\u00f6nen ve daha hafif olan y\u0131ld\u0131zdan madde \u00e7ekti\u011fini g\u00f6rebiliyoruz. Kara deli\u011fe d\u00fc\u015fen maddeyi son kez parlak optik ve X-\u0131\u015f\u0131n\u0131 radyasyonu \u015feklinde g\u00f6r\u00fcyoruz. Sistemden at\u0131lan g\u00f6reli jetlerin \u00e7\u0131kard\u0131\u011f\u0131 radyo dalgalar\u0131n\u0131 g\u00f6rebiliyoruz.\u201d <\/p>\n Bu jetleri takip eden ara\u015ft\u0131rmac\u0131lar, kara deli\u011fin d\u00f6nme ekseninin y\u00f6n\u00fcn\u00fc \u00e7ok kesin \u015fekilde belirlemeyi ba\u015fard\u0131. Refakat eden y\u0131ld\u0131zdan kara deli\u011fe d\u00fc\u015fen gaz miktar\u0131 sonradan azalmaya ba\u015flad\u0131k\u00e7a, y\u0131ld\u0131z\u0131n \u0131\u015f\u0131\u011f\u0131 s\u00f6n\u00fckle\u015fmi\u015f ve sistemdeki \u0131\u015f\u0131\u011f\u0131n b\u00fcy\u00fck bir b\u00f6l\u00fcm\u00fc refakat\u00e7i y\u0131ld\u0131zdan gelmeye ba\u015flad\u0131. Bilim insanlar\u0131 bu sayede tayf \u00f6l\u00e7\u00fcm y\u00f6ntemleri kullanarak y\u00f6r\u00fcnge e\u011fimini \u00f6l\u00e7meyi ba\u015fard\u0131. Ayr\u0131ca bu \u00f6l\u00e7\u00fcm\u00fcn, f\u0131rlat\u0131lan jetlerin e\u011fimiyle neredeyse \u00f6rt\u00fc\u015ft\u00fc\u011f\u00fc ifade edildi.<\/p>\n Kaynak: Popular Science T\u00fcrkiye<\/p>\n