Kozmik toz, y\u0131ld\u0131zlar\u0131n ve gezegenlerin olu\u015fumu i\u00e7in son derece \u00f6nemlidir; fakat gen\u00e7 evrende olduk\u00e7a fazla miktarda kozmik toz bulunuyor olmas\u0131, bug\u00fcne kadar gizemini koruyan bir s\u0131rd\u0131. Astronomlar bir s\u00fcpernovay\u0131 g\u00f6zlemleyerek evrenin b\u00fcy\u00fck b\u00f6l\u00fcm\u00fcn\u00fc olu\u015fturan tozun nereden geldi\u011fini \u00e7\u00f6zm\u00fc\u015f olabilirler.<\/p>\n
Y\u0131ld\u0131zlar\u0131n ve kat\u0131 y\u00fczeye sahip gezegenlerin do\u011fumunda \u00f6nemli rol oynayan ve ya\u015fam i\u00e7in gerekli olan elementsel i\u00e7eri\u011fi sa\u011flayan kozmik tozun k\u00f6keni bir muamma. Bir\u00e7ok astrofizik\u00e7i bu tozun y\u00fcksek k\u00fctleli ve k\u0131sa ya\u015fam s\u00fcresine sahip y\u0131ld\u0131zlar\u0131n \u00f6l\u00fcmleri anlam\u0131na gelen s\u00fcpernova patlamalar\u0131 s\u0131ras\u0131nda olu\u015ftu\u011fu g\u00f6r\u00fc\u015f\u00fcnde.<\/p>\n
Fakat galaksimiz yak\u0131nlar\u0131ndaki s\u00fcpernovalar \u00fczerinde yap\u0131lan baz\u0131 g\u00f6zlemler \u015funu g\u00f6steriyor ki; bu patlamalar sonucunda ortaya \u00e7\u0131kan malzeme, gen\u00e7 evreni kaplayan bol miktardaki tozu a\u00e7\u0131klayamayacak kadar az miktarda.<\/p>\n
Astronomlar, patlamas\u0131n\u0131n 2. haftas\u0131ndan itibaren tam 2,5 y\u0131l s\u00fcre ile bir s\u00fcpernovadaki tozun bile\u015fimini kaydederek, bu s\u0131rr\u0131n \u00fczerindeki perdeyi kald\u0131rd\u0131lar. \u00c7al\u0131\u015fma, patlayan y\u0131ld\u0131z\u0131n yaratt\u0131\u011f\u0131 \u015foka dayanabilen, iri yap\u0131l\u0131 toz zerrelerinin bile\u015fimlerini ortaya \u00e7\u0131kard\u0131. Sonu\u00e7lar toz \u00fcretiminin ba\u015flang\u0131\u00e7ta yava\u015f oldu\u011fu ve zamanla h\u0131zland\u0131\u011f\u0131n\u0131 g\u00f6steriyor.<\/p>\n
\u00d6nceden ger\u00e7ekle\u015ftirilen \u00e7al\u0131\u015fmalarda, her bir s\u00fcpernova k\u0131sa zaman periyotlar\u0131nda inceliyordu. Nature<\/em> dergisinde yay\u0131mlanan makalenin yazarlar\u0131ndan biri olan, Danimarka\u2019n\u0131n Aarhus \u00dcniversitesi\u2019nden astrofizik\u00e7i Christa Gall bununla ilgili olarak \u201cOnlar bize s\u00fcpernovalar\u0131n ne miktarda toz \u00fcretti\u011fiyle ilgili hik\u00e2yenin tamam\u0131n\u0131 anlatm\u0131yordu\u201d diyor.<\/p>\n Gall ve \u00e7al\u0131\u015fma arkada\u015flar\u0131, ilk kez 2010 y\u0131l\u0131nda yak\u0131nlardaki bir galakside oldu\u011fu tespit edilen SN 2010jl s\u00fcpernovas\u0131n\u0131 g\u00f6zlemledi.<\/p>\n I\u015f\u0131k ve \u0131s\u0131 <\/strong><\/p>\n \u015eili Cerro Paranal\u2019da bulunan nam-\u0131 di\u011fer \u00c7ok B\u00fcy\u00fck Teleskop\u2019un spektrograf\u0131n\u0131 kullanan ekip, toz par\u00e7ac\u0131klar\u0131 taraf\u0131ndan emilen g\u00f6r\u00fcn\u00fcr \u0131\u015f\u0131\u011f\u0131 ve yine bu par\u00e7ac\u0131klar\u0131n yay\u0131nlad\u0131\u011f\u0131 k\u0131z\u0131l\u00f6tesi tayf\u0131ndaki radyasyonu \u00f6l\u00e7t\u00fcler.<\/p>\n \u0130ngiltere\u2019nin Queen\u2019s \u00dcniversitesi\u2019nden astronom Rubina Kotak\u2019a g\u00f6re, ekibin elde etti\u011fi veriler \u00f6zellikle merak uyand\u0131r\u0131c\u0131; \u00e7\u00fcnk\u00fc bu veriler, patlama sonras\u0131ndaki haftalardan itibaren ge\u00e7en y\u0131llar zarf\u0131ndaki s\u00fcre\u00e7te e\u015fzamanl\u0131 olarak belirli bir dalga boyu aral\u0131\u011f\u0131na giren yay\u0131n alan\u0131n\u0131 i\u00e7eriyor. Bu veriler hem toz zerrelerinin boyutlar\u0131 hem de bile\u015fimiyle ilgili bilgi i\u00e7eriyor. \u201cBu t\u00fcr bir kapsam\u0131 elde etmek en yak\u0131ndaki ve en parlak s\u00fcpernova olaylar\u0131 hari\u00e7 son derece zor\u201d diyor Kotak.<\/p>\n Ekip patlamadan 40-240 g\u00fcn sonra g\u00f6r\u00fclen tozun s\u00fcpernova ger\u00e7ekle\u015fmeden \u00f6nce d\u0131\u015far\u0131ya at\u0131lm\u0131\u015f olan maddeden meydana gelmesi gerekti\u011fi sonucunu \u00e7\u0131kartt\u0131. Di\u011fer bir ihtimal ise toz y\u0131k\u0131nt\u0131s\u0131n\u0131n s\u00fcpernovan\u0131n kendisi taraf\u0131ndan y\u0131ld\u0131zlararas\u0131 ortama f\u0131rlat\u0131lm\u0131\u015f olmas\u0131. Fakat Gall\u2019in belirtti\u011fine g\u00f6re, patlaman\u0131n yaratt\u0131\u011f\u0131 s\u0131cakl\u0131k, maddelerin toz par\u00e7ac\u0131klar\u0131na yo\u011funla\u015fmas\u0131na imk\u00e2n tan\u0131mayacak kadar y\u00fcksek. Patlamadan sonraki s\u00fcre\u00e7te, s\u00fcpernovan\u0131n yaratt\u0131\u011f\u0131 geni\u015fleyen \u015fok dalgas\u0131 h\u0131zla ge\u00e7ip giderken, \u00f6nceden d\u0131\u015far\u0131 at\u0131lm\u0131\u015f malzemeyi so\u011fuk ve yo\u011fun bir kabu\u011fa s\u0131k\u0131\u015ft\u0131r\u0131r. Bu ortam toz partik\u00fcllerini kayna\u015ft\u0131rmak ve b\u00fcy\u00fctmek i\u00e7in ideal ko\u015fullar\u0131 sa\u011flar.<\/p>\n \u0130ri par\u00e7ac\u0131klar \u015fok dalgalar\u0131na dayan\u0131kl\u0131<\/strong><\/p>\n \u015ea\u015f\u0131rt\u0131c\u0131 olan astronomlar\u0131n buldu\u011fu toz par\u00e7ac\u0131klar\u0131n\u0131n Samanyolu standartlar\u0131na g\u00f6re \u00e7ok iri olmas\u0131yd\u0131. 1-4,2 mikrometre aras\u0131nda \u00f6l\u00e7\u00fclen boyutlara sahip bu par\u00e7ac\u0131klar, galaksimiz i\u00e7erisinde yer alan y\u0131ld\u0131z sistemleri aras\u0131ndaki toz par\u00e7ac\u0131klar\u0131n\u0131n en az 4 kat\u0131 geni\u015fli\u011fe sahip. Gall\u2019e g\u00f6re b\u00fcy\u00fck boyutlu toz par\u00e7ac\u0131klar\u0131n\u0131n olu\u015fmas\u0131, k\u00fc\u00e7\u00fck boyuttakilere g\u00f6re daha zor, fakat bu \u00f6zellikleri, onlar\u0131 s\u00fcpernovalardan kaynaklanan ve y\u0131ld\u0131zlararas\u0131 ortama \u00e7arpan \u015foklar\u0131n yaratt\u0131\u011f\u0131 y\u0131k\u0131ma kar\u015f\u0131 daha direngen yap\u0131yor. Bu par\u00e7ac\u0131klar\u0131n uzun \u00f6m\u00fcrl\u00fc olmas\u0131nda bu \u00f6zelliklerinin etkisi var.<\/p>\n \u0130lk g\u00f6zlemlerde SN 2010jl etraf\u0131ndaki toz miktar\u0131 g\u00f6receli olarak azd\u0131. G\u00fcne\u015f\u2019in k\u00fctlesinin 10 binde 1\u2019inden d\u00fc\u015f\u00fck seviyelerdeydi. Fakat patlamadan 500-868 g\u00fcn sonras\u0131nda bu miktar 10 kattan fazla artt\u0131.<\/p>\n Gall\u2019in belirtti\u011fine g\u00f6re, h\u0131zlanma miktar\u0131 s\u00fcpernovan\u0131n toz \u00fcretiminde ikinci bir faza ge\u00e7ildi\u011fini g\u00f6steriyor. S\u00fcpernova yeteri kadar so\u011fudu\u011fu s\u0131rada, bir kez karbonca zengin malzeme ve di\u011fer y\u0131k\u0131nt\u0131lar meydana geldi mi, tozun i\u00e7inde kayna\u015fma ba\u015fl\u0131yor ve \u00fcretim h\u0131zlan\u0131yor. 868. g\u00fcnde, yani Gall ve ekibinin s\u00fcpernovay\u0131 son g\u00f6zlemleyi\u015finde, gaz miktar\u0131 G\u00fcne\u015f\u2019in k\u00fctlesinin binde 2,5\u2019una, yani D\u00fcnya\u2019n\u0131n k\u00fctlesinin 830 kat\u0131na kar\u015f\u0131l\u0131k geliyordu.<\/p>\n E\u011fer artan toz \u00fcretimi b\u00f6yle devam ederse, t\u0131pk\u0131 SN 1987A s\u00fcpernovas\u0131nda g\u00f6zlendi\u011fi gibi, SN 2010jl de 20 y\u0131l i\u00e7erisinde G\u00fcne\u015f\u2019in k\u00fctlesinin yar\u0131s\u0131na kar\u015f\u0131l\u0131k gelecek miktarda toz par\u00e7ac\u0131\u011f\u0131 \u00fcretmi\u015f olacak. Gall\u2019e g\u00f6re e\u011fer erken evrende \u00e7ok say\u0131da s\u00fcpernova ayn\u0131 h\u0131zla kozmik toz \u00fcretimi yapm\u0131\u015f ise, bu s\u00fcre\u00e7 gen\u00e7 evreni kaplayan tozu a\u00e7\u0131klayabilir.<\/p>\n <\/p>\n","protected":false},"excerpt":{"rendered":" Kozmik toz, y\u0131ld\u0131zlar\u0131n ve gezegenlerin olu\u015fumu i\u00e7in son derece \u00f6nemlidir; fakat gen\u00e7 evrende olduk\u00e7a fazla miktarda kozmik toz bulunuyor olmas\u0131, bug\u00fcne kadar gizemini koruyan bir s\u0131rd\u0131. Astronomlar bir s\u00fcpernovay\u0131 g\u00f6zlemleyerek evrenin b\u00fcy\u00fck b\u00f6l\u00fcm\u00fcn\u00fc olu\u015fturan tozun nereden geldi\u011fini \u00e7\u00f6zm\u00fc\u015f olabilirler. Y\u0131ld\u0131zlar\u0131n ve kat\u0131 y\u00fczeye sahip gezegenlerin do\u011fumunda \u00f6nemli rol oynayan ve ya\u015fam i\u00e7in gerekli olan elementsel […]<\/p>\n","protected":false},"author":677,"featured_media":25328,"comment_status":"closed","ping_status":"closed","sticky":false,"template":"","format":"standard","meta":{"_acf_changed":false,"footnotes":""},"categories":[163,30,19],"tags":[248,657,293,3239],"class_list":["post-25327","post","type-post","status-publish","format-standard","has-post-thumbnail","hentry","category-126-sayi","category-astronomi","category-bilim-gundemi","tag-astronomi","tag-evren","tag-gezegenler","tag-yildiz-patlamasi"],"acf":[],"aioseo_notices":[],"aioseo_head":"\n\t\t\n\t\n\t\n\t\n\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t\n\t\t