Penn State’teki astronomi ve astrofizik doktora ara\u015ft\u0131rmac\u0131s\u0131 ve konu hakk\u0131ndaki makalenin ba\u015f yazar\u0131 Pragati Pradhan, “Y\u0131ld\u0131z r\u00fczgarlar\u0131 y\u0131ld\u0131zlardan \u00e7\u0131kan protonlar, elektronlar ve metal atomlar\u0131ndan olu\u015fan h\u0131zl\u0131 akan bir malzemedir. Bu malzeme y\u0131ld\u0131z\u0131n \u00e7evresini metallerle, kinetik enerjiyle ve iyonla\u015ft\u0131r\u0131c\u0131 radyasyonla zenginle\u015ftirir. Y\u0131ld\u0131zlar\u0131n olu\u015fmas\u0131 i\u00e7in gerekli en temel \u015feylerden biridir. Son on y\u0131la kadar, y\u0131ld\u0131z r\u00fczgarlar\u0131n\u0131n homojen yap\u0131da oldu\u011fu d\u00fc\u015f\u00fcn\u00fcl\u00fcyordu. Ancak Chandra G\u00f6zlemevi’nden ald\u0131\u011f\u0131m\u0131z veriler, bunun aksini kan\u0131tlad\u0131.” dedi.<\/p>\n
Olay\u0131n g\u00f6zlemlendi\u011fi sistemde iki adet y\u0131ld\u0131z bulunuyor; bunlardan birisi olduk\u00e7a k\u00fc\u00e7\u00fck ve yo\u011fun n\u00f6tron y\u0131ld\u0131z\u0131, di\u011feri de normal bir s\u00fcper dev. Bu iki y\u0131ld\u0131zl\u0131 sisteme yap\u0131lan g\u00f6zlemlerde, olmas\u0131 gerekenden farkl\u0131 bir durum fark eden ara\u015ft\u0131rmac\u0131lar, b\u00f6ylece y\u0131ld\u0131zlar\u0131n i\u00e7indeki n\u00f6tr demir atomlar\u0131n\u0131n olu\u015ftu\u011fu en d\u00fc\u015f\u00fck s\u0131n\u0131r\u0131 belirleyebildi: 2,5 \u0131\u015f\u0131k-saniyesi ya da 750 bin kilometre.<\/p>\n
N\u00f6tron y\u0131ld\u0131z\u0131, y\u0131ld\u0131zlar\u0131n ya\u015famlar\u0131n\u0131n son bulabilece\u011fi bi\u00e7imlerden biridir. Bir n\u00f6tron y\u0131ld\u0131z\u0131 dev bir y\u0131ld\u0131z Tip II, Tip Ib veya Tip Ic bir s\u00fcpernova olarak patlad\u0131ktan sonra geri kalan k\u0131sm\u0131n kendi i\u00e7ine \u00e7\u00f6kmesiyle olu\u015fur. Bu y\u0131ld\u0131zlar neredeyse tamamen n\u00f6tronlardan olu\u015fsa da az miktarda proton ve elektron da i\u00e7erir. Bu proton ve elektronlar olmadan n\u00f6tron y\u0131ld\u0131zlar\u0131 uzun s\u00fcre var olmaya devam edemezdi. \u00c7\u00fcnk\u00fc n\u00f6tronlar serbest haldeyken karars\u0131zd\u0131r ve beta \u0131\u015f\u0131mas\u0131 yaparak k\u0131sa s\u00fcre i\u00e7inde proton ve elektronlara ayr\u0131\u015f\u0131r. Ancak y\u0131ld\u0131z\u0131n i\u00e7indeki y\u00fcksek bas\u0131n\u00e7 sebebiyle proton ve elektronlar\u0131n birle\u015ferek n\u00f6tronlara d\u00f6n\u00fc\u015fmesi, n\u00f6tron y\u0131ld\u0131zlar\u0131n\u0131n daha kararl\u0131 bir yap\u0131ya sahip olmas\u0131n\u0131 sa\u011flar.<\/p>\n
N\u00f6tron y\u0131ld\u0131zlar\u0131n\u0131n k\u00fctleleri G\u00fcne\u015f\u2019inkinin 1,44 ila 3 kat\u0131 olabilir. Bug\u00fcne kadar g\u00f6zlemlenmi\u015f en b\u00fcy\u00fck n\u00f6tron y\u0131ld\u0131z\u0131n\u0131n k\u00fctlesi ise G\u00fcne\u015f\u2019inkinin yakla\u015f\u0131k iki kat\u0131d\u0131r. Samanyolu i\u00e7inde yakla\u015f\u0131k 2000 n\u00f6tron y\u0131ld\u0131z\u0131 oldu\u011fu biliniyor. G\u00fcne\u015f Sistemi\u2019ne en yak\u0131n n\u00f6tron y\u0131ld\u0131zlar\u0131, yakla\u015f\u0131k 400 \u0131\u015f\u0131k y\u0131l\u0131 uzakl\u0131ktaki RX J1856.5-3754 ve yakla\u015f\u0131k 424 \u0131\u015f\u0131k y\u0131l\u0131 uzakl\u0131ktaki PSR J0108-1431\u2019dir.<\/p>\n
N\u00f6tron y\u0131ld\u0131zlar\u0131n\u0131n k\u00fctleleri \u00e7ok b\u00fcy\u00fck olmas\u0131na ra\u011fmen hacimleri \u00e7ok k\u00fc\u00e7\u00fckt\u00fcr. \u00d6rne\u011fin k\u00fctlesi G\u00fcne\u015f\u2019inkinin yakla\u015f\u0131k 1,5 kat\u0131 olan bir n\u00f6tron y\u0131ld\u0131z\u0131n\u0131n \u00e7ap\u0131 sadece 10 kilometre civar\u0131ndad\u0131r. Bu durum n\u00f6tron y\u0131ld\u0131zlar\u0131n\u0131n yo\u011funluklar\u0131n\u0131n \u00e7ok y\u00fcksek olmas\u0131na neden olur. \u00d6yle ki n\u00f6tron y\u0131ld\u0131zlar\u0131n\u0131n yo\u011funluklar\u0131 G\u00fcne\u015f\u2019inkinin 2,6 x 1014 ila 4,1 x 1014 kat\u0131d\u0131r.<\/p>\n
N\u00f6tron y\u0131ld\u0131zlar\u0131n\u0131n k\u00fctle\u00e7ekimi etkisiyle daha fazla k\u00fc\u00e7\u00fclmemelerinin nedeni, Pauli d\u0131\u015farlama ilkesidir. Bu ilke, fermiyon grubu iki par\u00e7ac\u0131\u011f\u0131n -\u00f6rne\u011fin protonlar, elektronlar ve n\u00f6tronlar- ayn\u0131 konuma ve ayn\u0131 kuantum durumuna sahip olamayaca\u011f\u0131n\u0131 s\u00f6yler. Bu y\u00fczden k\u00fctlesi G\u00fcne\u015f\u2019inkinin \u00fc\u00e7 kat\u0131ndan az olan n\u00f6tron y\u0131ld\u0131zlar\u0131n\u0131n yo\u011funlu\u011fu atom \u00e7ekirde\u011findeki yo\u011funluklar d\u00fczeyine ula\u015ft\u0131\u011f\u0131 zaman \u00e7\u00f6kme durur. Ancak k\u00fctlesi G\u00fcne\u015f\u2019inkinin be\u015f kat\u0131ndan fazla olan n\u00f6tron y\u0131ld\u0131zlar\u0131 karars\u0131zd\u0131r ve \u00e7\u00f6kmeye devam ederler. Bu y\u0131ld\u0131zlar karadeli\u011fe d\u00f6n\u00fc\u015f\u00fcr.
\nBilinen n\u00f6tron y\u0131ld\u0131zlar\u0131n\u0131n yakla\u015f\u0131k %5\u2019i ikili y\u0131ld\u0131z sistemlerinin \u00fcyeleridir. Bu sistemlerdeki n\u00f6tron y\u0131ld\u0131zlar\u0131n\u0131n e\u015fleri normal y\u0131ld\u0131zlar, beyaz c\u00fcceler ya da ba\u015fka n\u00f6tron y\u0131ld\u0131zlar\u0131 olabilir. Genel g\u00f6relilik kuram\u0131, ikili y\u0131ld\u0131z sistemlerinin k\u00fctle\u00e7ekimsel dalgalar yayaca\u011f\u0131n\u0131 ve zaman i\u00e7inde y\u0131ld\u0131zlar aras\u0131ndaki mesafenin azalaca\u011f\u0131n\u0131 s\u00f6yler. K\u00fctle\u00e7ekimsel dalgalar\u0131n varl\u0131\u011f\u0131 ile ilgili ilk kan\u0131t, n\u00f6tron y\u0131ld\u0131z\u0131 i\u00e7eren bir ikili y\u0131ld\u0131z sisteminin g\u00f6zlemlenmesi ve y\u0131ld\u0131zlar aras\u0131ndaki mesafenin genel g\u00f6relilik kuram\u0131n\u0131n tahminleriyle uyumlu bir bi\u00e7imde de\u011fi\u015fti\u011finin bulunmas\u0131yla elde edildi.<\/p>\n","protected":false},"excerpt":{"rendered":"
Penn State’teki astronomi ve astrofizik doktora ara\u015ft\u0131rmac\u0131s\u0131 ve konu hakk\u0131ndaki makalenin ba\u015f yazar\u0131 Pragati Pradhan, “Y\u0131ld\u0131z r\u00fczgarlar\u0131 y\u0131ld\u0131zlardan \u00e7\u0131kan protonlar, elektronlar ve metal atomlar\u0131ndan olu\u015fan h\u0131zl\u0131 akan bir malzemedir. Bu malzeme y\u0131ld\u0131z\u0131n \u00e7evresini metallerle, kinetik enerjiyle ve iyonla\u015ft\u0131r\u0131c\u0131 radyasyonla zenginle\u015ftirir. Y\u0131ld\u0131zlar\u0131n olu\u015fmas\u0131 i\u00e7in gerekli en temel \u015feylerden biridir. Son on y\u0131la kadar, y\u0131ld\u0131z r\u00fczgarlar\u0131n\u0131n homojen […]<\/p>\n","protected":false},"author":23,"featured_media":0,"comment_status":"closed","ping_status":"closed","sticky":false,"template":"","format":"standard","meta":{"_acf_changed":false,"inline_featured_image":false,"footnotes":""},"categories":[506],"tags":[],"class_list":["post-49957","post","type-post","status-publish","format-standard","hentry","category-astronomi"],"acf":[],"yoast_head":"\n