{"id":22064,"date":"2015-03-01T16:09:58","date_gmt":"2015-03-01T14:09:58","guid":{"rendered":"https:\/\/bilimvegelecek.com.tr\/?p=22064"},"modified":"2018-03-19T16:52:00","modified_gmt":"2018-03-19T13:52:00","slug":"kara-madde-nedir","status":"publish","type":"post","link":"https:\/\/bilimvegelecek.com.tr\/index.php\/2015\/03\/01\/kara-madde-nedir","title":{"rendered":"Kara madde nedir?"},"content":{"rendered":"<p><em>Kara maddeyi belirlemek i\u00e7in fizik\u00e7ilerin en \u00e7ok umut ba\u011flad\u0131klar\u0131 yakla\u015f\u0131m, erken evrenin \u00e7ok y\u00fcksek s\u0131cakl\u0131k ve yo\u011funluk durumunu yeniden yaratan y\u00fcksek enerjili \u00e7arp\u0131\u015fmalard\u0131r. Kara madde par\u00e7ac\u0131klar\u0131n\u0131n ger\u00e7ekten bu ko\u015fullar alt\u0131nda \u00fcretilip \u00fcretilmedi\u011fini g\u00f6rmek i\u00e7in CERN ve benzeri laboratuar ko\u015fullar\u0131nda evrenin ilk durumu yeniden olu\u015fturulmaktad\u0131r. <\/em><\/p>\n<p>G\u00fcn\u00fcm\u00fczde yan\u0131t arayan \u00f6nemli bir kozmolojik problem <strong>kara madde<\/strong>nin kayna\u011f\u0131d\u0131r. G\u00f6zlemlenebilir evrende yap\u0131lan \u00f6l\u00e7\u00fcmler, galaksilerin hesaplanabilen maddeden daha fazla bir maddenin \u00e7ekim etkisi y\u00fcz\u00fcnden \u00e7ok h\u0131zl\u0131 d\u00f6nd\u00fcklerini ortaya \u00e7\u0131karm\u0131\u015ft\u0131r. Kayna\u011f\u0131n\u0131 bilmedi\u011fimiz bu maddeye <strong>kara madde<\/strong> ad\u0131n\u0131 vermekteyiz. Bu ba\u011flamda kara madde<strong> \u00e7ekici<\/strong> bir g\u00fc\u00e7t\u00fcr ve evrenin i\u00e7e \u00e7\u00f6kmesini art\u0131ran bir etki yapar.<\/p>\n<p>\u00d6ncelikle kafa kar\u0131\u015ft\u0131r\u0131c\u0131 bir noktay\u0131 a\u00e7\u0131kl\u0131\u011fa kavu\u015ftural\u0131m: <strong>kara madde<\/strong> ve <strong>kara enerji<\/strong> olarak bilinen bu iki bile\u015fen, ikisinin birbirleriyle ili\u015fkili oldu\u011fu izlenimi uyand\u0131r\u0131r ama tek ortak noktalar\u0131 \u0131\u015f\u0131\u011f\u0131 so\u011furmamalar\u0131 ve yaymamalar\u0131d\u0131r. Kara madde ve kara enerjinin fiziksel \u00f6zellikleri ile evren tarihindeki i\u015flevleri tamamen farkl\u0131d\u0131r.<\/p>\n<p><strong>Kara maddenin ke\u015ffi<\/strong><\/p>\n<p>Ne oldu\u011funu h\u00e2l\u00e2 bilmedi\u011fimiz kara maddenin ke\u015ffi dedektif \u00f6yk\u00fclerine benzer. Kara madde ilk olarak, 1930 y\u0131l\u0131nda California Teknoloji Enstit\u00fcs\u00fc\u2019nde \u00e7al\u0131\u015fan bir astronom olan ve galaksi k\u00fcmelerindeki galaksilerin h\u0131zl\u0131 hareketlerini anlamaya \u00e7al\u0131\u015fan Fritz Zwicky taraf\u0131ndan saptand\u0131. Zwicky, d\u00fcnyadan milyonlarca \u0131\u015f\u0131k y\u0131l\u0131 uzakl\u0131ktaki galaksilerin, \u0131\u015f\u0131k yayan maddenin yaratabilece\u011fi ku\u0308tle\u00e7ekimle a\u00e7\u0131klanamayacak kadar h\u0131zl\u0131 hareket ettiklerini fark etti. Dolay\u0131s\u0131yla, bu galaksilerin etraflar\u0131nda \u0131\u015f\u0131k yaymayan ama galaksileri kuramsal olarak hesaplanandan \u00e7ok daha h\u0131zl\u0131 d\u00f6nd\u00fcrmek i\u00e7in gerekli olan ku\u0308tle\u00e7ekimi sa\u011flayan fazladan madde olmal\u0131yd\u0131. Yap\u0131lan hesaplar, galaksilerin ku\u0308tlelerinin bu\u0308yu\u0308k \u00e7o\u011funlu\u011funun bu \u0131\u015f\u0131k sa\u00e7mayan madde olmas\u0131 gerekti\u011fini g\u00f6sterdi.<\/p>\n<p>Zwicky\u2019nin ke\u015ffi hemen kabul g\u00f6rmediyse de, 1970\u2019lere gelindi\u011finde art\u0131k galaksinin y\u0131ld\u0131zlar\u0131n\u0131n ince bir disk i\u00e7inde tutunabilmesi i\u00e7in b\u00fcy\u00fck bir kara madde bulutu i\u00e7ine g\u00f6m\u00fclm\u00fc\u015f olmas\u0131 gerekti\u011fi anla\u015f\u0131lm\u0131\u015ft\u0131. Bu konuda en ikna edici \u00e7al\u0131\u015fmalar\u0131 Carnegie Enstit\u00fcs\u00fc\u2019nden Vera Rubin ve Kent Ford ger\u00e7ekle\u015ftirdi. Rubin ve \u00e7al\u0131\u015fma arkada\u015flar\u0131n\u0131n bulgular\u0131 galaksilerdeki g\u00f6r\u00fclebilen maddenin, en h\u0131zl\u0131 hareket eden y\u0131ld\u0131zlar\u0131n galaksiden kurtulmas\u0131n\u0131 engelleyebilecek k\u00fctle\u00e7ekimi \u00fcretemeyece\u011fini a\u00e7\u0131k\u00e7a ortaya koyuyordu. Dolay\u0131s\u0131yla astronomlar evrenin y\u0131ld\u0131z olu\u015fturmayan, \u0131\u015f\u0131k yaymayan ama k\u00fctle\u00e7ekim kuvveti uygulayan bir madde t\u00fcr\u00fcyle -kara madde- dolu olmas\u0131 gerekti\u011fi sonucuna vard\u0131lar. Evrenimizin \u0131\u015f\u0131k yayan bile\u015fenleri olan y\u0131ld\u0131zlar, kara madde okyanusundaki planktonlara benziyordu.<\/p>\n<p>Ancak o g\u00fcn bug\u00fcnd\u00fcr (yakla\u015f\u0131k 85 y\u0131ld\u0131r) kara maddenin ne oldu\u011fu anla\u015f\u0131lamad\u0131. Pek \u00e7ok aday \u00f6ne s\u00fcr\u00fcld\u00fc: Devasa kara delikler, dev gezegenler, tan\u0131mlanamayan g\u00f6k sicimleri vs. Ancak b\u00fct\u00fcn bu adaylar elendi. 1970\u2019ler, 80\u2019ler ve 90\u2019lar kara madde avc\u0131l\u0131\u011f\u0131yla ge\u00e7ti. Bu s\u00fcre\u00e7te fizik\u00e7iler kara madde hakk\u0131nda \u00e7ok say\u0131da veri toplad\u0131lar. \u00d6rne\u011fin 1980\u2019lerde astronomlar ilk kez, k\u00fctle\u00e7ekim alan\u0131n\u0131n i\u00e7inden ge\u00e7en \u0131\u015f\u0131k \u0131\u015f\u0131nlar\u0131n\u0131n nas\u0131l e\u011fildi\u011fini g\u00f6zlemleyerek, k\u00fctle\u00e7ekimsel mercek etkisi yoluyla galaksi k\u00fcmeleri i\u00e7indeki kara maddeyi \u201cg\u00f6rmeye\u201d ba\u015flad\u0131lar. T\u0131pk\u0131 tamamen \u015feffaf olan bir bardak suyun i\u00e7inden ge\u00e7en \u0131\u015f\u0131\u011f\u0131n b\u00fck\u00fcl\u00fcp arkas\u0131ndaki g\u00f6r\u00fcnt\u00fcy\u00fc sapt\u0131rmas\u0131 gibi, bir galaksi k\u00fcmesi i\u00e7indeki kara madde tamamen saydam olsa da, k\u00fctle\u00e7ekim etkisi nedeniyle uzak bir galaksiden d\u00fcnyaya do\u011fru gelen \u0131\u015f\u0131\u011f\u0131 i\u00e7inden ge\u00e7erken b\u00fcker. Dolay\u0131s\u0131yla kara madde, bir k\u00fctle\u00e7ekimsel mercek olarak davranabilir: Teleskop g\u00f6r\u00fcnt\u00fcs\u00fcnde galaksilerin merceklenmi\u015f ve sapt\u0131r\u0131lm\u0131\u015f \u015fekilleri, yak\u0131n galaksi k\u00fcmelerinin g\u00f6r\u00fcnt\u00fcleriymi\u015f gibi ortaya \u00e7\u0131kabilir. Bu verilerin analiz edilmesiyle astronomlar kara maddenin \u00f6zelliklerini saptad\u0131lar ve merceklenmi\u015f g\u00f6r\u00fcnt\u00fc motifleri ile b\u00fck\u00fclen \u0131\u015f\u0131\u011f\u0131n modellenmesi sayesinde, galaksi k\u00fcmesi i\u00e7indeki kara madde da\u011f\u0131l\u0131m\u0131n\u0131 ortaya koydular. Yap\u0131lan b\u00fct\u00fcn bu ara\u015ft\u0131rmalar ve g\u00f6zlemler, kara maddenin evrenin kritik yo\u011funlu\u011fun yakla\u015f\u0131k yu\u0308zde 25\u2019i kadar\u0131n\u0131 meydana getirdi\u011fini ortaya koymaktad\u0131r. G\u00f6r\u00fcnen maddenin yu\u0308zde 5\u2019iyle birlikte kara madde, standart kozmolojinin \u00f6ng\u00f6rd\u00fc\u011f\u00fc miktar\u0131n yu\u0308zde 30\u2019unu a\u00e7\u0131klamakta. Geriye kalan y\u00fczde 70\u2019lik k\u0131sm\u0131n ne oldu\u011fuysa ancak 1998\u2019de kara enerjinin ke\u015ffiyle anla\u015f\u0131ld\u0131.<\/p>\n<p><strong>Evrenin tarihinde kara maddenin \u00f6nemi<\/strong><\/p>\n<p>Her ne kadar kayna\u011f\u0131n\u0131n ne oldu\u011fu tam olarak anla\u015f\u0131lmam\u0131\u015f olsa da, astronomlar g\u00fcn\u00fcm\u00fczde kara maddeyi daha iyi anlamaya ba\u015flad\u0131lar. B\u00fcy\u00fck patlamadan sonra, evrenin s\u0131cak plazmayla dolu oldu\u011fu d\u00f6nemlerde, \u0131\u015f\u0131n\u0131m\u0131n \u015fiddetli bas\u0131nc\u0131 atom \u00e7ekirdekleri ve elektronlardan olu\u015fan s\u0131radan maddeyi birbirleriyle k\u00fcmele\u015fmelerinden korumu\u015ftu. Ancak kara madde \u0131\u015f\u0131kla (fotonlarla) etkile\u015fmedi\u011fi ve \u0131\u015f\u0131n\u0131m taraf\u0131ndan etkilenmedi\u011fi i\u00e7in, yo\u011funla\u015farak kara madde bulutlar\u0131n\u0131 olu\u015fturmakta serbestti. B\u00fcy\u00fck patlamadan 380 bin y\u0131l sonra ilk atomlar olu\u015fmaya ba\u015flad\u0131\u011f\u0131nda evren \u0131\u015f\u0131n\u0131m\u0131n bask\u0131nl\u0131\u011f\u0131ndan kurtulacak ve s\u0131radan madde de k\u00fcmele\u015fmeye ba\u015flayacakt\u0131. Bu d\u00f6nemde evren, elektron ile proton ve n\u00f6tronlar\u0131n birle\u015ferek y\u00fcks\u00fcz atomlar olu\u015fturmas\u0131na yetecek kadar so\u011fudu\u011funda s\u0131radan madde \u0131\u015f\u0131n\u0131m\u0131n etkisinden kurtuldu. Evrende kara madde k\u00fcmeleri zaten mevcuttu ve galaksileri, y\u0131ld\u0131zlar\u0131 ve gezegenleri olu\u015fturduklar\u0131 s\u0131radan maddeyi \u00e7ekirdeklerine \u00e7ekecek kadar yo\u011funla\u015fm\u0131\u015flard\u0131. Bu nedenle, e\u011fer kara madde olmasayd\u0131 galaksiler daha nadir ortaya \u00e7\u0131karlard\u0131: uzay\u0131n \u00e7o\u011funda kara enerji bulunurdu ve maddeyi k\u00fcmele\u015fmeden \u00f6nce seyreltirdi. Galaksiler olmadan da y\u0131ld\u0131z ve gezegen var olamazd\u0131. Dolay\u0131s\u0131yla, hen\u00fcz ne oldu\u011funu bilmesek de, asl\u0131nda hepimiz varl\u0131\u011f\u0131m\u0131z\u0131 kara maddeye bor\u00e7luyuz.<\/p>\n<p><strong>G\u00fcn\u00fcm\u00fczde kara madde ara\u015ft\u0131rmalar\u0131<\/strong><\/p>\n<p>Kara maddenin kayna\u011f\u0131 konusunda yap\u0131lan 40-50 y\u0131ll\u0131k ara\u015ft\u0131rmalar sonunda art\u0131k b\u00fcy\u00fck boyutlu adaylardan vazge\u00e7ildi. Neredeyse b\u00fct\u00fcn fizik\u00e7iler kara maddenin elektriksel olarak y\u00fcks\u00fcz olan ve bu nedenle s\u0131radan maddeyle \u00e7ok zay\u0131f etkile\u015fen ve \u0131\u015f\u0131k sa\u00e7mayan ya da so\u011furmayan bir temel par\u00e7ac\u0131k olmas\u0131 gerekti\u011fi konusunda hemfikir. Bu nedenle kara madde aray\u0131\u015flar\u0131 uzaydan yery\u00fcz\u00fcne indi. H\u0131zland\u0131r\u0131c\u0131 deneylerinde kara madde aranmas\u0131na ba\u015fland\u0131. \u00d6rne\u011fin e\u011fer n\u00f6trinolar\u0131n k\u00fctlesi daha fazla olsayd\u0131 iyi bir kara madde aday\u0131 olurdu. N\u00f6trinolar, s\u0131radan maddeyle \u00e7ok zay\u0131f etkile\u015firler ve \u0131\u015f\u0131k sa\u00e7mazlar ya da so\u011furmazlar. Ancak k\u00fctleleri o kadar azd\u0131r ki, Standart Modelde yap\u0131lan baz\u0131 hesaplamalarda n\u00f6trino k\u00fctlesi s\u0131f\u0131r kabul edilir. Ne yaz\u0131k ki, n\u00f6trinolar\u0131n k\u00fctlesi kara maddeyi a\u00e7\u0131klamakta yetersizdir.<\/p>\n<p>Kara maddeyi belirlemenin bir di\u011fer yolu, bunlar\u0131 do\u011frudan saptamaya yetecek duyarl\u0131l\u0131kta aletler tasarlamakt\u0131r. Bu ama\u00e7la fizik\u00e7iler dedekt\u00f6rleri, y\u00fcksek enerjili kozmik \u0131\u015f\u0131nlardan korumak i\u00e7in madenlerin derinliklerine yerle\u015ftirirler ve b\u00f6ylece bir kara madde par\u00e7ac\u0131\u011f\u0131n\u0131n bir atom \u00e7ekirde\u011fiyle \u00e7arp\u0131\u015farak iyonize olmu\u015f par\u00e7ac\u0131klar\u0131n ve \u0131\u015f\u0131\u011f\u0131n iz b\u0131rakt\u0131\u011f\u0131 birka\u00e7 nadir olay\u0131 ara\u015ft\u0131rmaktalar. Ancak \u015fimdiye dek ger\u00e7ekle\u015ftirilen pek \u00e7ok deneyde kara maddeyi do\u011frulayan herhangi bir saptama olmad\u0131.<\/p>\n<p>Kara maddeyi belirlemek i\u00e7in fizik\u00e7ilerin en \u00e7ok umut ba\u011flad\u0131klar\u0131 yakla\u015f\u0131m, erken evrenin \u00e7ok y\u00fcksek s\u0131cakl\u0131k ve yo\u011funluk durumunu yeniden yaratan y\u00fcksek enerjili \u00e7arp\u0131\u015fmalard\u0131r. Kara madde par\u00e7ac\u0131klar\u0131n\u0131n ger\u00e7ekten bu ko\u015fullar alt\u0131nda \u00fcretilip \u00fcretilmedi\u011fini g\u00f6rmek i\u00e7in CERN ve benzeri laboratuar ko\u015fullar\u0131nda evrenin ilk durumu yeniden olu\u015fturulmaktad\u0131r.<\/p>\n<p><strong>Kara madde ve s\u00fcpersimetri<\/strong><\/p>\n<p>CERN\u2019deki LHC (B\u00fcy\u00fck Hadron \u00c7arp\u0131\u015f\u0131t\u0131r\u0131c\u0131s\u0131) h\u0131zland\u0131r\u0131c\u0131s\u0131nda konu\u015flanan iki b\u00fcy\u00fck deneyde (ATLAS ve CMS) Higgs par\u00e7ac\u0131\u011f\u0131n\u0131n yan\u0131 s\u0131ra kara madde adaylar\u0131 da ara\u015ft\u0131r\u0131l\u0131yor. 2012 y\u0131l\u0131nda Higgs par\u00e7ac\u0131\u011f\u0131n\u0131n ke\u015ffiyle birlikte art\u0131k kara madde adaylar\u0131 ara\u015ft\u0131rmalar\u0131 \u00f6n plana \u00e7\u0131kt\u0131. Bunlardan en pop\u00fcleri s\u00fcpersimetrik par\u00e7ac\u0131klard\u0131r. \u00d6ncelikle s\u00fcpersimetrinin ne oldu\u011funu anlamaya \u00e7al\u0131\u015fal\u0131m. E\u011fer Higgs bozonu temel bir par\u00e7ac\u0131ksa, iki se\u00e7enek vard\u0131r: \u0130lki, \u00e7ok gizemli bir \u015fekilde, skalar Higgs alan\u0131na kuplaj yapan daha a\u011f\u0131r herhangi bir par\u00e7ac\u0131\u011f\u0131n var olmamas\u0131 gerekti\u011fidir; ikinci se\u00e7enek ise, Higgs k\u00fctlesine yap\u0131lan d\u00fczeltmelerde bir \u015fekilde birbirini g\u00f6t\u00fcren terimler var olmal\u0131d\u0131r. Bu ise ancak bir <strong>simetri <\/strong>ile olanakl\u0131d\u0131r. Bu durumda <strong>fermiyonlar<\/strong> ile <strong>bozonlar\u0131<\/strong> birbirlerine ba\u011flayan bir simetrinin varl\u0131\u011f\u0131 ka\u00e7\u0131n\u0131lmaz g\u00f6z\u00fckmektedir. E\u011fer Standart Model\u2019in kuarklar\u0131 ve leptonlar\u0131 iki kompleks skalarla (<strong>s\u00fcper-e\u015fler<\/strong>) birlikte ortaya \u00e7\u0131karlarsa, t\u00fcm s\u00fcper-e\u015flerin daha hafif s\u00fcper-e\u015flere do\u011fru bozunan karars\u0131z par\u00e7ac\u0131klar olmas\u0131 beklenir; bunun istisnas\u0131 en hafif s\u00fcper-e\u015fdir (<strong>LSP<\/strong>), \u00e7\u00fcnk\u00fc onun bozunup d\u00f6n\u00fc\u015fece\u011fi daha hafif par\u00e7ac\u0131\u011f\u0131 yoktur ve dolay\u0131s\u0131yla kararl\u0131d\u0131r. Bunun sonucu olarak s\u00fcpersimetri evrene yeni bir kararl\u0131 par\u00e7ac\u0131k katar ve bu par\u00e7ac\u0131k fotonlara, elektronlara, n\u00f6trinolara ve protonlara eklenir. Y\u0131ld\u0131zlar\u0131n g\u00f6rd\u00fc\u011f\u00fcm\u00fcz \u0131\u015f\u0131\u011f\u0131 fotonlardan olu\u015fur. Protonlar ve elektronlar y\u0131ld\u0131zlar\u0131 ve gezegenleri olu\u015fturur. N\u00f6trinolar ve LSP (varsa) evren boyunca mevcut olan madde bi\u00e7imleri olacakt\u0131r. Sadece zay\u0131f ve k\u00fctle \u00e7ekimsel kuvvetleri hissettiklerinden, elektromanyetik ya da ye\u011fin kuvvetleri hissetmediklerinden, y\u0131ld\u0131zlar\u0131n olu\u015fumuna kat\u0131lmayacaklar,<strong> kara m<\/strong><strong>adde<\/strong> olacaklard\u0131r. S\u00fcpersimetri, LSP\u2019den olu\u015fan kara maddenin var oldu\u011funu \u00f6ng\u00f6r\u00fcr.<\/p>\n<p>B\u00fcy\u00fck patlaman\u0131n hemen sonras\u0131nda, her par\u00e7ac\u0131k t\u00fcr\u00fcnden yakla\u015f\u0131k olarak ayn\u0131 say\u0131da vard\u0131. Evren geni\u015fleyip so\u011furken \u00e7o\u011fu par\u00e7ac\u0131k daha hafif par\u00e7ac\u0131klar halinde bozundu ve kimileri de yok olarak di\u011ferlerine d\u00f6n\u00fc\u015ft\u00fc. Hepsinin nas\u0131l etkile\u015fti\u011fi hakk\u0131nda bir teorimiz var, b\u00f6ylece \u015fimdi geriye ka\u00e7 tanesinin kald\u0131\u011f\u0131n\u0131 hesaplayabiliriz. G\u00f6rebilece\u011fimiz fotonlar \u00fcreten y\u0131ld\u0131zlar halinde topla\u015fm\u0131\u015f olmasalar da, yeterli miktardaysalar g\u00f6rebildiklerimize uygulad\u0131klar\u0131 k\u00fctle \u00e7ekim yoluyla varl\u0131klar\u0131 tespit edilebilir; varl\u0131klar\u0131 y\u0131ld\u0131zlar\u0131n galaksilerin i\u00e7indeki hareket \u015feklini ve galaksilerin birbirine g\u00f6re nas\u0131l hareket etti\u011fini de\u011fi\u015fikli\u011fe u\u011frat\u0131r. 1980\u2019lerin ilk yar\u0131s\u0131nda s\u00fcpersimetrinin, y\u0131ld\u0131zlardaki maddeden bile kayda de\u011fer \u00f6l\u00e7\u00fcde daha fazla LSP (kara madde) \u00f6ng\u00f6rd\u00fc\u011f\u00fc fark edildi. S\u00fcpersimetrinin yeni fikirler ve yakla\u015f\u0131m y\u00f6ntemleri sundu\u011fu temel konular aras\u0131nda, evrenin nas\u0131l olup da as\u0131l olarak <strong>kar\u015f\u0131-madde<\/strong> de\u011fil de madde halinde olu\u015ftu\u011fu (CP simetrisinin ihlali), protonlar\u0131n bozunup bozunmad\u0131\u011f\u0131 ve bozunuyorlarsa nas\u0131l bozunduklar\u0131, evrenin neden \u015fimdiki ya\u015f\u0131nda ve boyutunda oldu\u011fu ve kuarklar\u0131n ve leptonlar\u0131n bozunumlar\u0131n\u0131n enderli\u011fi, yer al\u0131r.<\/p>\n<p>B\u00fct\u00fcn bu nedenlerden dolay\u0131, CERN\u2019deki LHC deneylerinde ba\u015fta gelen ara\u015ft\u0131rmalar s\u00fcpersimetrik par\u00e7ac\u0131klar\u0131n ke\u015ffine yo\u011funla\u015fm\u0131\u015f durumda. Hen\u00fcz s\u00fcpersimetrik par\u00e7ac\u0131klar g\u00f6zlemlenemedi, ancak LHC deneylerindeki ara\u015ft\u0131rmalar 20-30 y\u0131l kadar devam edecek.<\/p>\n","protected":false},"excerpt":{"rendered":"<p>Kara maddeyi belirlemek i\u00e7in fizik\u00e7ilerin en \u00e7ok umut ba\u011flad\u0131klar\u0131 yakla\u015f\u0131m, erken evrenin \u00e7ok y\u00fcksek s\u0131cakl\u0131k ve yo\u011funluk durumunu yeniden yaratan y\u00fcksek enerjili \u00e7arp\u0131\u015fmalard\u0131r. Kara madde par\u00e7ac\u0131klar\u0131n\u0131n ger\u00e7ekten bu ko\u015fullar alt\u0131nda \u00fcretilip \u00fcretilmedi\u011fini g\u00f6rmek i\u00e7in CERN ve benzeri laboratuar ko\u015fullar\u0131nda evrenin ilk durumu yeniden olu\u015fturulmaktad\u0131r. G\u00fcn\u00fcm\u00fczde yan\u0131t arayan \u00f6nemli bir kozmolojik problem kara maddenin kayna\u011f\u0131d\u0131r. G\u00f6zlemlenebilir [&hellip;]<\/p>\n","protected":false},"author":380,"featured_media":22065,"comment_status":"closed","ping_status":"closed","sticky":false,"template":"","format":"standard","meta":{"_acf_changed":false,"footnotes":""},"categories":[170,1464,26],"tags":[657,2680,2681,2682],"class_list":["post-22064","post","type-post","status-publish","format-standard","has-post-thumbnail","hentry","category-133-sayi","category-dosya","category-fizik","tag-evren","tag-kara-enerji","tag-kara-madde","tag-supersimetri"],"acf":[],"aioseo_notices":[],"aioseo_head":"\n\t\t<!-- All in One SEO 4.9.8 - aioseo.com -->\n\t<meta name=\"robots\" content=\"max-image-preview:large\" \/>\n\t<meta name=\"author\" content=\"Prof. Dr. Kerem Canko\u00e7ak\"\/>\n\t<link rel=\"canonical\" href=\"https:\/\/bilimvegelecek.com.tr\/index.php\/2015\/03\/01\/kara-madde-nedir\" \/>\n\t<meta name=\"generator\" content=\"All in One SEO (AIOSEO) 4.9.8\" \/>\n\t\t<meta property=\"og:locale\" content=\"tr_TR\" \/>\n\t\t<meta property=\"og:site_name\" content=\"Bilim ve Gelecek\" \/>\n\t\t<meta property=\"og:type\" content=\"article\" \/>\n\t\t<meta property=\"og:title\" content=\"Kara madde nedir? | Bilim ve Gelecek\" \/>\n\t\t<meta property=\"og:url\" content=\"https:\/\/bilimvegelecek.com.tr\/index.php\/2015\/03\/01\/kara-madde-nedir\" \/>\n\t\t<meta property=\"fb:app_id\" content=\"2104805563100892\" \/>\n\t\t<meta property=\"fb:admins\" content=\"1250955469\" \/>\n\t\t<meta property=\"og:image\" content=\"https:\/\/bilimvegelecek.com.tr\/wp-content\/uploads\/2018\/03\/karamadde-foto.jpg\" \/>\n\t\t<meta property=\"og:image:secure_url\" content=\"https:\/\/bilimvegelecek.com.tr\/wp-content\/uploads\/2018\/03\/karamadde-foto.jpg\" \/>\n\t\t<meta property=\"og:image:width\" content=\"800\" \/>\n\t\t<meta property=\"og:image:height\" content=\"450\" \/>\n\t\t<meta property=\"article:published_time\" content=\"2015-03-01T14:09:58+00:00\" \/>\n\t\t<meta property=\"article:modified_time\" content=\"2018-03-19T13:52:00+00:00\" \/>\n\t\t<meta property=\"article:publisher\" content=\"https:\/\/www.facebook.com\/bilimvegelecekdergisi\/\" \/>\n\t\t<meta name=\"twitter:card\" content=\"summary\" \/>\n\t\t<meta name=\"twitter:site\" content=\"@bilimvegelecek\" \/>\n\t\t<meta name=\"twitter:title\" content=\"Kara madde nedir? | Bilim ve Gelecek\" \/>\n\t\t<meta name=\"twitter:image\" content=\"https:\/\/bilimvegelecek.com.tr\/wp-content\/uploads\/2018\/03\/karamadde-foto.jpg\" \/>\n\t\t<script type=\"application\/ld+json\" class=\"aioseo-schema\">\n\t\t\t{\"@context\":\"https:\\\/\\\/schema.org\",\"@graph\":[{\"@type\":\"Article\",\"@id\":\"https:\\\/\\\/bilimvegelecek.com.tr\\\/index.php\\\/2015\\\/03\\\/01\\\/kara-madde-nedir#article\",\"name\":\"Kara madde nedir? | Bilim ve Gelecek\",\"headline\":\"Kara madde nedir?\",\"author\":{\"@id\":\"https:\\\/\\\/bilimvegelecek.com.tr\\\/index.php\\\/author\\\/kcankocak#author\"},\"publisher\":{\"@id\":\"https:\\\/\\\/bilimvegelecek.com.tr\\\/#organization\"},\"image\":{\"@type\":\"ImageObject\",\"url\":\"https:\\\/\\\/bilimvegelecek.com.tr\\\/wp-content\\\/uploads\\\/2018\\\/03\\\/karamadde-foto.jpg\",\"width\":800,\"height\":450},\"datePublished\":\"2015-03-01T16:09:58+02:00\",\"dateModified\":\"2018-03-19T16:52:00+03:00\",\"inLanguage\":\"tr-TR\",\"mainEntityOfPage\":{\"@id\":\"https:\\\/\\\/bilimvegelecek.com.tr\\\/index.php\\\/2015\\\/03\\\/01\\\/kara-madde-nedir#webpage\"},\"isPartOf\":{\"@id\":\"https:\\\/\\\/bilimvegelecek.com.tr\\\/index.php\\\/2015\\\/03\\\/01\\\/kara-madde-nedir#webpage\"},\"articleSection\":\"133. 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