Onlarca y\u0131ld\u0131r s\u00fcren karanl\u0131k madde ara\u015ft\u0131rmalar\u0131, genellikle karanl\u0131k maddenin ne olamayaca\u011f\u0131na dair \u00e7\u0131karsamalar \u00fcretiyor. Ancak bu art\u0131k de\u011fi\u015fmi\u015f olabilir: \u00c7arp\u0131\u015fmakta olan d\u00f6rt galaksi \u00fczerinde yap\u0131lan yeni \u00e7al\u0131\u015fma, ilk kez normal maddenin etkilenmedi\u011fi; sadece karanl\u0131k maddenin kat\u0131ld\u0131\u011f\u0131 ve k\u00fctle\u00e7ekimsel olmayan bir etkile\u015fmenin varl\u0131\u011f\u0131n\u0131 savl\u0131yor. Bulgular evrenin y\u00fczde 24\u2019\u00fcn\u00fc olu\u015fturan karanl\u0131k madde i\u00e7in \u00f6nemli nitelikte olabilir. E\u011fer sonu\u00e7lar do\u011fruysa karanl\u0131k madde anlay\u0131\u015f\u0131m\u0131z t\u00fcm\u00fcyle de\u011fi\u015fecek.<\/p>\n
Olgular\u0131 a\u00e7\u0131klayan en basit mekanizma, bilimde \u00f6ncelikli tercihtir. Ayn\u0131 olguyu ba\u015far\u0131yla a\u00e7\u0131klayan karma\u015f\u0131k tezler elenirken, basit olanlar ge\u00e7erlilik kazan\u0131r. Ayn\u0131 \u015fekilde kendi i\u00e7inde etkile\u015fen karanl\u0131k madde tezi, daha \u00f6nceleri ortaya at\u0131lm\u0131\u015f olsa da, Occam\u2019\u0131n usturas\u0131n\u0131n keskin taraf\u0131yla kar\u015f\u0131la\u015fm\u0131\u015f ve kabul g\u00f6rmemi\u015ftir. Nas\u0131l ki baryonik etkile\u015fmelerin ger\u00e7ekle\u015febilmesi i\u00e7in temel kuvvetler ve kuvvet ta\u015f\u0131y\u0131c\u0131 bozonlar mevcut ise, karanl\u0131k maddenin kendi i\u00e7erisinde etkile\u015fime girmesi de beraberinde yeni bir \u201ckaranl\u0131k kuvvet<\/strong>\u201d ve kuvvet ta\u015f\u0131y\u0131c\u0131 \u201ckaranl\u0131k bozon<\/strong>\u201d gerektirir. B\u00f6yle bir karma\u015faya girmek yerine tek par\u00e7ac\u0131ktan meydana gelen, madde ve kendi aras\u0131nda \u00e7ok nadir etkile\u015fen veya hi\u00e7 etkile\u015fmeyen karanl\u0131k madde modeli benimsenmi\u015f ve ana ak\u0131m a\u00e7\u0131klama bi\u00e7imi olmu\u015ftur.<\/p>\n \u015eili\u2019de bulunan Very Large Telescope\u2019nin MUSE (\u00e7ok \u00fcniteli spektroskopik g\u00f6zleyici) enstr\u00fcman\u0131 ve bununla birlikte Hubble Uzay Teleskobu kullan\u0131larak yap\u0131lan yeni \u00e7al\u0131\u015fmada ise Abell 3827 galaksi k\u00fcmesindeki d\u00f6rt galaksinin \u00e7arp\u0131\u015fmas\u0131 g\u00f6zlemlenerek, karanl\u0131k kuvvet ve karanl\u0131k bozonun var olabilece\u011fine dair sinyaller ilk kez raporland\u0131.<\/p>\n G\u00f6r\u00fcnmez karanl\u0131k maddeyi tespit edebilmek i\u00e7in genel g\u00f6relili\u011fin \u00f6ng\u00f6rd\u00fc\u011f\u00fc fiziksel fenomen olan k\u00fctle\u00e7ekimsel merceklenmeden<\/strong> yararlan\u0131ld\u0131. Merceklenme, k\u00fctlenin uzay-zaman\u0131 b\u00fckt\u00fc\u011f\u00fc durumlarda ger\u00e7ekle\u015fir: K\u00fctle, adeta bir mercek gibi davran\u0131r ve b\u00fckt\u00fc\u011f\u00fc uzay\u0131n yak\u0131n\u0131ndan ge\u00e7en \u0131\u015f\u0131\u011f\u0131 odaklar. Normalde bize ula\u015fmamas\u0131 gereken g\u00f6kcisimlerinden gelen \u0131\u015f\u0131k, k\u00fctle\u00e7ekimsel merceklenmeyle bize ula\u015fabilir.<\/p>\n Abell 3827, karanl\u0131k maddenin yo\u011fun, dolay\u0131s\u0131yla uzay-zaman b\u00fck\u00fclmesinin de fazla oldu\u011fu bir galaksi k\u00fcmesidir. K\u00fcmenin arkas\u0131ndaki uzak mesafelerden gelen \u0131\u015f\u0131k, k\u00fcme taraf\u0131ndan b\u00fck\u00fclmeye u\u011frayarak D\u00fcnya\u2019ya ula\u015f\u0131r. I\u015f\u0131\u011f\u0131n b\u00fck\u00fclme a\u00e7\u0131lar\u0131ndan faydalanarak da k\u00fcmenin i\u00e7erdi\u011fi karanl\u0131k madde miktar\u0131 hakk\u0131nda bilgi sahibi olunabilir. Bahsi ge\u00e7en \u00e7al\u0131\u015fmada, \u00e7arp\u0131\u015fan galaksilerden en az birindeki karanl\u0131k maddenin, galaksideki y\u0131ld\u0131z ve di\u011fer bilindik maddeden 5000 \u0131\u015f\u0131k y\u0131l\u0131 mesafeyle ayr\u0131\u015ft\u0131\u011f\u0131 g\u00f6zlemlendi. Ayr\u0131\u015fman\u0131n a\u00e7\u0131klamas\u0131 ise karanl\u0131k maddenin di\u011fer galaksilerdeki karanl\u0131k maddeyle etkile\u015fime girerek yava\u015flad\u0131\u011f\u0131 ve bu \u015fekilde normal maddenin arkas\u0131nda kald\u0131\u011f\u0131 \u015feklinde yap\u0131ld\u0131. Mekanizma ayn\u0131 olsa da karanl\u0131k madde herhangi bir elektromanyetik etkile\u015fmeye girmez; bu itimi sa\u011flayabilecek tek kuvvet, yeni bir karanl\u0131k kuvvet ve kuvvet par\u00e7ac\u0131\u011f\u0131 olmal\u0131d\u0131r.<\/p>\n \u00c7al\u0131\u015fman\u0131n \u00f6nc\u00fcleri, sonu\u00e7lar kar\u015f\u0131s\u0131nda olduk\u00e7a temkinli. Tak\u0131m \u00fcyesi David Harvey, \u201cBu olduk\u00e7a heyecan verici. \u0130lk kez k\u00fctle\u00e7ekimsel olmayan bir etkile\u015fme g\u00f6zlenmi\u015f olabilir. Ancak yine de daha fazla obje \u00fczerinde g\u00f6zlem yap\u0131lmas\u0131 gerek\u201d diyor ve g\u00f6zlemlerinin hen\u00fcz kan\u0131tlanmad\u0131\u011f\u0131n\u0131 yineliyor. Bulgular\u0131n ba\u015fka olas\u0131 a\u00e7\u0131klamalar\u0131 da olabilir: Teleskoplarda g\u00f6zlenen desenlere D\u00fcnya\u2019n\u0131n g\u00f6r\u00fc\u015f a\u00e7\u0131s\u0131nda olmayan ba\u015fka bir k\u00fcmedeki karanl\u0131k maddenin sebep olmas\u0131 olas\u0131l\u0131klar dahilinde.<\/p>\n Kendi i\u00e7inde etkile\u015fen karanl\u0131k madde, karanl\u0131k kuvvet ve karanl\u0131k foton modelinin, klasik tek par\u00e7ac\u0131k a\u00e7\u0131klamas\u0131 kadar basit de\u011fil, fakat olduk\u00e7a makul oldu\u011funu d\u00fc\u015f\u00fcnen Weiner, \u201cKaranl\u0131k maddenin kendi i\u00e7inde etkile\u015fti\u011fi fikrine bizi y\u00f6nlendiren temel motivasyon noktas\u0131 standart model oldu. Standart model i\u00e7erisinde farkl\u0131 etkile\u015fim kuvvetleri ve farkl\u0131 arac\u0131 par\u00e7ac\u0131klar var. Bu bak\u0131\u015f a\u00e7\u0131s\u0131yla karanl\u0131k maddenin de kendi etkile\u015fim kuvvetlerinin olmas\u0131 do\u011fal g\u00f6z\u00fck\u00fcyor\u201d diyor.<\/p>\n Mekanizma ayn\u0131 zamanda tek par\u00e7ac\u0131k modelinin \u00f6ng\u00f6r\u00fcleri ile g\u00f6zlemler aras\u0131ndaki uyu\u015fmazl\u0131\u011f\u0131 da ortadan kald\u0131r\u0131yor. \u00d6rne\u011fin tek par\u00e7ac\u0131k modeli galaksi merkezlerinin daha yo\u011fun olmas\u0131 gerekti\u011fini savlamaktad\u0131r. Kendi i\u00e7inde etkile\u015fen karanl\u0131k madde ise galaktik merkezde \u00e7arp\u0131\u015f\u0131p merkezden uzakla\u015fabilir. B\u00f6ylece g\u00f6zlenen merkezsel seyrekli\u011fe mant\u0131kl\u0131 bir a\u00e7\u0131klama da getirilmi\u015f olur.<\/p>\n \u015eimdiye dek galaksi \u00e7arp\u0131\u015fmalar\u0131 g\u00f6zlemlerinde kendi i\u00e7inde etkile\u015fen karanl\u0131k madde g\u00f6zlemlenemedi. Karanl\u0131k maddenin varl\u0131\u011f\u0131na dair ilk g\u00fc\u00e7l\u00fc delillerden birini sunan, olduk\u00e7a yo\u011fun galaksi \u00e7arp\u0131\u015fmalar\u0131n\u0131n meydana geldi\u011fi Bullet k\u00fcmesinde yap\u0131lan k\u00fctle\u00e7ekimsel merceklenme g\u00f6zlemleri, karanl\u0131k maddenin g\u00f6r\u00fcn\u00fcr maddeden ayr\u0131\u015ft\u0131\u011f\u0131n\u0131 ortaya koymu\u015ftu; fakat karanl\u0131k maddenin kendi i\u00e7erisinde etkile\u015fime girdi\u011fini savlayacak yeterli bir ayr\u0131\u015fma g\u00f6zlemlememi\u015fti. Ancak 2006\u2019daki Bullet k\u00fcmesi \u00e7al\u0131\u015fmalar\u0131nda bulunmu\u015f Maru\u0161a Brada\u010d, yeni sonu\u00e7lar\u0131n Bullet k\u00fcmesi sonu\u00e7lar\u0131yla \u00e7eli\u015fmedi\u011fini vurguluyor. Yak\u0131n zamanda yap\u0131lan bir ba\u015fka \u00e7al\u0131\u015fmada ise 72 galaksi k\u00fcmesi \u00e7arp\u0131\u015fmas\u0131 g\u00f6zlemlenmi\u015f ve yine kendi i\u00e7erisinde etkile\u015fen karanl\u0131k maddeye dair herhangi bir iz bulunamam\u0131\u015ft\u0131r. Fakat dikkat edilmesi gereken \u00f6nemli bir nokta ise, Bullet ve di\u011fer \u00e7al\u0131\u015fmada Abell 3827\u2019deki gibi galaksilerin de\u011fil galaksi k\u00fcmesi \u00e7arp\u0131\u015fmalar\u0131n\u0131n g\u00f6zlemlenmi\u015f oldu\u011fu. Galaksilerin \u00e7arp\u0131\u015fmalar\u0131, k\u00fcmelerin \u00e7arp\u0131\u015fmalar\u0131ndan g\u00f6rece daha yava\u015f olur. Etkile\u015fime girebilmek i\u00e7in yeterli zaman\u0131 k\u00fcme \u00e7arp\u0131\u015fmalar\u0131nda bulamayan karanl\u0131k madde, galaksi \u00e7arp\u0131\u015fmalar\u0131nda bulabilir. Dolay\u0131s\u0131yla do\u011fru s\u0131namalar\u0131n galaksi k\u00fcmelerinden de\u011fil, galaksilerden gelmesi gerekir. \u201c\u0130nceledi\u011fimiz di\u011fer k\u00fcmelerdeki galaksilerde de \u00e7arp\u0131\u015fmalar mevcut, fakat hi\u00e7biri Abell 3827\u2019deki kadar i\u015fe yarar nitelikte de\u011fil\u201d diyen Harvey, gelecekte yap\u0131lacak g\u00f6zlemlerin yeni galaksi \u00e7arp\u0131\u015fmalar\u0131n\u0131 ortaya \u00e7\u0131karaca\u011f\u0131ndan umutlu.<\/p>\n","protected":false},"excerpt":{"rendered":" Onlarca y\u0131ld\u0131r s\u00fcren karanl\u0131k madde ara\u015ft\u0131rmalar\u0131, genellikle karanl\u0131k maddenin ne olamayaca\u011f\u0131na dair \u00e7\u0131karsamalar \u00fcretiyor. Ancak bu art\u0131k de\u011fi\u015fmi\u015f olabilir: \u00c7arp\u0131\u015fmakta olan d\u00f6rt galaksi \u00fczerinde yap\u0131lan yeni \u00e7al\u0131\u015fma, ilk kez normal maddenin etkilenmedi\u011fi; sadece karanl\u0131k maddenin kat\u0131ld\u0131\u011f\u0131 ve k\u00fctle\u00e7ekimsel olmayan bir etkile\u015fmenin varl\u0131\u011f\u0131n\u0131 savl\u0131yor. Bulgular evrenin y\u00fczde 24\u2019\u00fcn\u00fc olu\u015fturan karanl\u0131k madde i\u00e7in \u00f6nemli nitelikte olabilir. E\u011fer […]<\/p>\n","protected":false},"author":634,"featured_media":20892,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"_acf_changed":false,"footnotes":""},"categories":[173,30,19,26],"tags":[248,657,288,2517,1084,1161],"class_list":["post-2706","post","type-post","status-publish","format-standard","has-post-thumbnail","hentry","category-136-sayi","category-astronomi","category-bilim-gundemi","category-fizik","tag-astronomi","tag-evren","tag-fizik","tag-karanlik-kuvvet","tag-karanlik-madde","tag-kutlecekim"],"acf":[],"aioseo_notices":[],"_links":{"self":[{"href":"https:\/\/bilimvegelecek.com.tr\/index.php\/wp-json\/wp\/v2\/posts\/2706","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/bilimvegelecek.com.tr\/index.php\/wp-json\/wp\/v2\/posts"}],"about":[{"href":"https:\/\/bilimvegelecek.com.tr\/index.php\/wp-json\/wp\/v2\/types\/post"}],"author":[{"embeddable":true,"href":"https:\/\/bilimvegelecek.com.tr\/index.php\/wp-json\/wp\/v2\/users\/634"}],"replies":[{"embeddable":true,"href":"https:\/\/bilimvegelecek.com.tr\/index.php\/wp-json\/wp\/v2\/comments?post=2706"}],"version-history":[{"count":0,"href":"https:\/\/bilimvegelecek.com.tr\/index.php\/wp-json\/wp\/v2\/posts\/2706\/revisions"}],"wp:featuredmedia":[{"embeddable":true,"href":"https:\/\/bilimvegelecek.com.tr\/index.php\/wp-json\/wp\/v2\/media\/20892"}],"wp:attachment":[{"href":"https:\/\/bilimvegelecek.com.tr\/index.php\/wp-json\/wp\/v2\/media?parent=2706"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/bilimvegelecek.com.tr\/index.php\/wp-json\/wp\/v2\/categories?post=2706"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/bilimvegelecek.com.tr\/index.php\/wp-json\/wp\/v2\/tags?post=2706"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}
\nBenzer etkile\u015fme birbiri yak\u0131n\u0131ndan ge\u00e7en iki protonda g\u00f6zlenebilir: Elektromanyetik etkile\u015fme par\u00e7ac\u0131\u011f\u0131 olan foton arac\u0131l\u0131\u011f\u0131 ile protonlar birbirine itici kuvvet uygular.<\/p>\n