\n<\/p>\n
NASA\u2019n\u0131n Chandra X-I\u015f\u0131n\u0131 G\u00f6zlemevi ve VLA (Very Large Array) radyo teleskobundan elde edilen yeni verilere g\u00f6re, Samanyolu\u2019nun merkezindeki s\u00fcper k\u00fctleli kara delik<\/a> Sagittarius A* (Sgr A*), o kadar h\u0131zl\u0131 d\u00f6n\u00fcyor ki, etraf\u0131ndaki uzay<\/a>-zaman dokusunu e\u011fip b\u00fck\u00fcyor.<\/p>\n Bilim insanlar\u0131, kara deli\u011fin bu d\u00f6n\u00fc\u015f h\u0131z\u0131n\u0131n onu rugby topuna benzer bir \u015fekle soktu\u011funu s\u00f6yl\u00fcyor.<\/p>\n Astronomlara g\u00f6re \u00e7o\u011fu b\u00fcy\u00fck galaksinin merkezinde bir s\u00fcper k\u00fctleli kara delik bulunuyor; Samanyolu da buna dahil. Sagittarius A*, G\u00fcne\u015f\u2019in yakla\u015f\u0131k 4 milyon kat\u0131 k\u00fctleye sahip.<\/p>\n Kara deliklerin davran\u0131\u015flar\u0131n\u0131 anlamak i\u00e7in bilim insanlar\u0131 genellikle iki temel \u00f6zelli\u011fe bak\u0131yor: K\u00fctleleri ve d\u00f6nme h\u0131zlar\u0131 (spinleri). Ancak Sagittarius A* \u00fczerine yap\u0131lan \u00f6nceki \u00e7al\u0131\u015fmalar, d\u00f6n\u00fc\u015f h\u0131z\u0131 konusunda farkl\u0131 sonu\u00e7lara ula\u015fm\u0131\u015ft\u0131; baz\u0131lar\u0131 hi\u00e7 d\u00f6nmedi\u011fini, baz\u0131lar\u0131 ise maksimum h\u0131zda d\u00f6nd\u00fc\u011f\u00fcn\u00fc \u00f6ne s\u00fcrm\u00fc\u015ft\u00fc.<\/p>\n Ara\u015ft\u0131rmac\u0131lar, X-\u0131\u015f\u0131n\u0131 ve radyo dalgas\u0131 verilerini kullanarak kara deli\u011fin \u00e7evresindeki maddenin nas\u0131l hareket etti\u011fini inceledi.<\/p>\n Sonu\u00e7lara g\u00f6re Sagittarius A* maksimum olas\u0131 a\u00e7\u0131sal h\u0131z\u0131n y\u00fczde 60\u2019\u0131 kadar bir h\u0131zla d\u00f6n\u00fcyor. Maksimum a\u00e7\u0131sal momentumun ise y\u00fczde 90\u2019\u0131na sahip.<\/p>\n Bu da, kara deli\u011fin uzay-zaman\u0131 g\u00fc\u00e7l\u00fc bi\u00e7imde b\u00fckt\u00fc\u011f\u00fcn\u00fc ve etraf\u0131ndaki maddeyi etkiledi\u011fini g\u00f6steriyor.<\/p>\n Ara\u015ft\u0131rmayla birlikte payla\u015f\u0131lan bir \u00e7izimde, kara deli\u011fin \u00e7evresindeki uzay-zaman, oval bir yap\u0131 \u015feklinde betimleniyor. Sar\u0131 b\u00f6lgeler, kara deli\u011fe do\u011fru s\u00fcr\u00fcklenen gaz\u0131 temsil ediyor. O oval \u015feklin i\u00e7inde ama olay ufkunun d\u0131\u015f\u0131nda kalan b\u00f6lge \u201cbo\u015fluk (cavity)\u201d olarak adland\u0131r\u0131l\u0131yor. Mavi noktalar ise kara deli\u011fin kutuplar\u0131ndan \u0131\u015f\u0131k h\u0131z\u0131na yak\u0131n h\u0131zlarla f\u0131rlayan jetleri simgeliyor.<\/p>\n D\u00f6nen s\u00fcper k\u00fctleli kara delikler, \u00e7evrelerindeki maddeyle etkile\u015fime girerek plazma jetleri olu\u015fturabiliyor.<\/p>\n Sgr A* son birka\u00e7 bin y\u0131ld\u0131r nispeten sessiz olsa da, \u00e7evresindeki madde yo\u011funlu\u011fu artarsa bu durum de\u011fi\u015febilir ve kara delik yeniden aktif hale gelebilir.<\/p>\n<\/div>\nYEN\u0130 ARA\u015eTIRMA NE G\u00d6STERD\u0130?<\/strong><\/h3>\n
NEDEN \u00d6NEML\u0130?<\/strong><\/h3>\n