{"id":19470,"date":"2015-08-01T16:22:17","date_gmt":"2015-08-01T13:22:17","guid":{"rendered":"http:\/\/109.232.216.219\/~bilimvegelecek\/?p=19470"},"modified":"2018-02-14T16:50:18","modified_gmt":"2018-02-14T13:50:18","slug":"parcacik-fizikcileriyle-evrenbilimcilerin-mutlu-beraberligi-bosanmayla-mi-sonuclanacak","status":"publish","type":"post","link":"https:\/\/bilimvegelecek.com.tr\/index.php\/2015\/08\/01\/parcacik-fizikcileriyle-evrenbilimcilerin-mutlu-beraberligi-bosanmayla-mi-sonuclanacak","title":{"rendered":"Par\u00e7ac\u0131k fizik\u00e7ileriyle evrenbilimcilerin \u2018mutlu beraberli\u011fi\u2019 bo\u015fanmayla m\u0131 sonu\u00e7lanacak?"},"content":{"rendered":"

Karanl\u0131k erke yaln\u0131zca g\u00f6kbilim g\u00f6zlemleriyle ara\u015ft\u0131r\u0131labilecek derin ve ilgin\u00e7 bir sorunsald\u0131r. Ancak bu sorunsal bir\u00e7ok ilgin\u00e7 sorunsaldan yaln\u0131zca bir tanesidir ve \u201c\u00e7\u00f6z\u00fcm\u00fc\u201d \u00e7ok d\u00fc\u015f\u00fck olas\u0131l\u0131kla yap\u0131labilecektir. Karanl\u0131k erkenin s\u0131n\u0131rlar\u0131 belirlenebilir, bu konudaki olas\u0131l\u0131klar\u0131n \u00e7o\u011fu d\u0131\u015flanabilir, ancak bir\u00e7o\u011fu da varl\u0131\u011f\u0131n\u0131 s\u00fcrd\u00fcrecektir. Karanl\u0131k erkenin b\u00fcy\u00fcleyici bir sorunsal oldu\u011fu yads\u0131namaz, ancak bu y\u00fcksek erke fizi\u011finin sorunsal\u0131d\u0131r. G\u00f6kbilimciler olarak astrofizi\u011fin ilgi alanlar\u0131ndan vazge\u00e7ip karanl\u0131k erkenin temel do\u011fas\u0131 sorunsal\u0131yla kand\u0131r\u0131lmamal\u0131y\u0131z.<\/em><\/p>\n

Sunu\u015f<\/strong><\/p>\n

Almanya\u2019n\u0131n Garching bei M\u00fcnchen Kenti\u2019ndeki Max Planck Enstit\u00fcs\u00fc Astrofizik B\u00f6l\u00fcm\u00fc y\u00f6neticisi olan Simon D. M. White\u2019\u0131n, Reports on Progress in Physics <\/em>(70, s.883-897, 2007) dergisinde \u201cK\u00f6ktenci fizik: Karanl\u0131k erke g\u00f6kbilim i\u00e7in neden k\u00f6t\u00fcd\u00fcr\u201d (\u201cFundamentalist physics: why Dark Energy is bad for astronomy\u201d) ba\u015fl\u0131kl\u0131 bir makalesi yay\u0131mlan\u0131yor. Bir\u00e7ok \u00f6d\u00fcl sahibi ve bilimler akademi \u00fcyesi olan White, karanl\u0131k erke (enerji) sorunsal\u0131 ile ilgili ilgin\u00e7 saptamalarda bulunuyor.<\/p><\/blockquote>\n

Simon D. M. White 30 Eyl\u00fcl 1951 y\u0131l\u0131nda \u0130ngiltere Kent Eyaleti Ashford \u015eehri\u2019nde d\u00fcnyaya gelmi\u015ftir. Yazar\u0131n SAO\/NASA Astrophysical Data Systems (ADS) sayfalar\u0131nda \u00e7ok say\u0131da (723) makalesi g\u00f6r\u00fcn\u00fcyor. Makalelerin \u00e7o\u011fu ApJ<\/em>, AJ<\/em>, MNRAS<\/em>, A<\/em>&A<\/em> gibi birinci s\u0131n\u0131f dergilerde yay\u0131mlanm\u0131\u015f. Makalelerin en eskisi 1975 y\u0131l\u0131nda ApJ<\/em> de \u201cUBV Photometry of NGC 2439\u201d; ADS sayfalar\u0131ndaki son makalesi de MNRAS<\/em> 2015 \u201cSurface photometry of brightest cluster galaxies and intracluster stars in LambdaCDM\u201d. 2015 y\u0131l\u0131ndaki makale say\u0131s\u0131 30! Makalelerine ald\u0131\u011f\u0131 at\u0131f say\u0131s\u0131 93066!<\/p>\n

Yazar\u0131n ilgi alan\u0131: g\u00f6kadalar\u0131n yap\u0131s\u0131, olu\u015fumu, evrimi ve k\u00fcmelenmesi; karanl\u0131k \u00f6zdek (madde), karanl\u0131k erke; kozmik yap\u0131 olu\u015fumlar\u0131n\u0131n \u00f6yk\u00fcn\u00fcm\u00fc (simulation); evrenbilim. \u00c7al\u0131\u015fmalar\u0131n\u0131 s\u00fcrd\u00fcrd\u00fc\u011f\u00fc g\u00f6zlemevleri: David Dunlap, Las Campanas, Wisw, Palomar, Lick, Steward and Multi-Mirror Telescope, Kit Peak National, La Palma, Einstein and ROSAT X-Ray uydular\u0131, ESO, VLT\/UT1, ISAAC, VLT\/UT2, FORS2.<\/p>\n

\"\"
Simon D. M. White.<\/figcaption><\/figure>\n

Simon D. M. White bir\u00e7ok \u00f6d\u00fcl\u00fcn yan\u0131 s\u0131ra, 1997 y\u0131l\u0131nda \u0130ngiliz Kraliyet Toplulu\u011fu\u2019na, 2005 y\u0131l\u0131nda Alman Ulusal Akademisi\u2019ne, 2007 y\u0131l\u0131nda ABD Ulusal Bilimler Akademisi\u2019ne \u00fcye se\u00e7ilmi\u015ftir. Amerikan Astronomi Toplulu\u011fu\u2019ndan Helen B. Warner \u00d6d\u00fcl\u00fc; Amerika Fizik Enstit\u00fcs\u00fc ve Amerika Astronomi Toplulu\u011fu\u2019ndan Dannie Heineman \u00d6d\u00fcl\u00fc ve \u0130ngiliz Kraliyet Astronomi Toplulu\u011fu\u2019ndan Alt\u0131n Madalya alm\u0131\u015ft\u0131r.<\/p>\n

White\u2019\u0131n \u201cK\u00f6ktenci fizik: Karanl\u0131k erke g\u00f6kbilim i\u00e7in neden k\u00f6t\u00fcd\u00fcr\u201d ba\u015fl\u0131kl\u0131 yaz\u0131s\u0131n\u0131 sunuyoruz.<\/p>\n

G\u00f6kbilimciler evrenimizdeki \u00e7e\u015fitli s\u00fcre\u00e7leri ve g\u00f6kcisimlerini g\u00f6zler. Y\u00fcksek erke fizik\u00e7ileriyse, uzay, zaman ve \u00f6zde\u011fin temel nedenlerini ortaya \u00e7\u0131karacak olan deneyler yaparak temel kuram<\/strong>\u0131n (\u201cfundamental theory\u201d) g\u00f6zlemlerle tutarl\u0131l\u0131\u011f\u0131n\u0131 s\u0131nar. Karanl\u0131k erke<\/strong> bu iki farkl\u0131 ara\u015ft\u0131rma alan\u0131 aras\u0131ndaki \u00f6zg\u00fcn ili\u015fkiyi olu\u015fturur. Karanl\u0131k erke temel kuram\u0131n en ince ayr\u0131nt\u0131lar\u0131n\u0131 yans\u0131t\u0131r ve varl\u0131\u011f\u0131 yaln\u0131zca g\u00f6kbilim alan\u0131nda yap\u0131lan g\u00f6zlemlerle kan\u0131tlanabilir. S\u00f6z\u00fc edilen ara\u015ft\u0131rma alanlar\u0131nda \u00e7al\u0131\u015fanlar, g\u00f6kbilimciler ve par\u00e7ac\u0131k fizik\u00e7ileri, karanl\u0131k erkenin s\u0131n\u0131rlar\u0131n\u0131 belirleyecek g\u00f6kbilim projelerini destekliyor. Ancak Simon D. M. White bu alandaki yak\u0131nla\u015fman\u0131n g\u00f6kbilime zarar verece\u011fini ileri s\u00fcr\u00fcyor:<\/p>\n

G\u00f6kbilim ve par\u00e7ac\u0131k fizi\u011fi de\u011fi\u015fik y\u00f6ntemleri ve de\u011fi\u015fik k\u00fclt\u00fcrleri olan ara\u015ft\u0131rma alanlar\u0131d\u0131r. G\u00f6kbilimciler kendilerine yabanc\u0131 bir ara\u015ft\u0131rma alan\u0131n\u0131n y\u00f6ntemlerini ele\u015ftirel olmayan bir yakla\u015f\u0131mla benimseyerek \u015fu an ba\u015far\u0131yla s\u00fcrd\u00fcrd\u00fckleri \u00e7al\u0131\u015fmalar\u0131n\u0131 ve bu \u00e7al\u0131\u015fmalar\u0131n gelecekteki canl\u0131l\u0131\u011f\u0131n\u0131 tehlikeye at\u0131yorlar. Karanl\u0131k erke ku\u015fkusuz g\u00f6kbilim g\u00f6zlemleriyle ara\u015ft\u0131r\u0131labilecek ilgin\u00e7 sorunsallardan yaln\u0131zca birisidir ve bu alana yap\u0131lan b\u00fcy\u00fck yat\u0131r\u0131mlar \u00f6nemli bir ilerlemenin ger\u00e7ekle\u015fece\u011fi anlam\u0131na gelmez.<\/p>\n

Hemen hemen tekd\u00fcze da\u011f\u0131l\u0131m g\u00f6steren karanl\u0131k erke alan\u0131, g\u00fcn\u00fcm\u00fcz evreninin erke yo\u011funlu\u011funda bask\u0131n olan etmendir ve evrenin giderek ivmeli geni\u015flemesinin nedenidir. Bu niteli\u011fiyle astrofizik\u00e7ilerin ve y\u00fcksek erke fizik\u00e7ilerinin ortak ilgi alan\u0131n\u0131 olu\u015fturuyor. Karanl\u0131k erkenin g\u00f6r\u00fcn\u00fcrdeki ve \u00f6zellikle de son derece d\u00fc\u015f\u00fck erke \u00f6l\u00e7eklerindeki \u00f6zellikleri, standart modelin ve onun bir uzant\u0131s\u0131 olan s\u00fcpersicim kuram\u0131n\u0131n \u00f6ng\u00f6remedi\u011fi bir durumdur. Bu durum \u00e7o\u011fu ara\u015ft\u0131rmac\u0131ya g\u00f6re karanl\u0131k erkenin \u00e7ekim ile di\u011fer kuvvetlerin birle\u015fimini yans\u0131tt\u0131\u011f\u0131na i\u015faret ediyor. K\u0131sacas\u0131, karanl\u0131k erkenin g\u00fcn\u00fcm\u00fcz h\u0131zland\u0131r\u0131c\u0131lar\u0131n eri\u015fti\u011fi erke d\u00fczeyinin olduk\u00e7a \u00fczerinde olmas\u0131 laboratuvarlarda g\u00f6zlenemeyece\u011fine i\u015faret eder.<\/p>\n

\u00d6yle g\u00f6r\u00fcn\u00fcyor ki, karanl\u0131k erkenin \u00f6zellikleri ancak g\u00f6kbilimsel g\u00f6zlemlerle ve \u00f6zellikle de evrenin g\u00fcn\u00fcm\u00fczde g\u00f6zlenen geni\u015flemesi ve kozmik yap\u0131lar\u0131n b\u00fcy\u00fcmesiyle belirlenebilir. B\u00f6ylesi \u00f6l\u00e7\u00fcmler \u00e7ok say\u0131da g\u00f6kadalar, g\u00f6kada k\u00fcmeleri ve s\u00fcpernovalar gibi karma\u015f\u0131k yap\u0131lar\u0131n g\u00f6zlemlerini gerektiriyor. Sonu\u00e7ta, s\u00fcpernovalar ve kozmik yap\u0131lar\u0131n olu\u015fumuyla ilgilenen g\u00f6kbilimciler, karanl\u0131k erkeye ili\u015fkin gereksinim duyulan kesin \u00f6zelliklerin sergilenmesi i\u00e7in par\u00e7ac\u0131k fizik\u00e7ileri ve astrofizik\u00e7i evrenbilimciler ile ortak proje tasarl\u0131yorlar. B\u00f6ylesi bir i\u015fbirli\u011fi, her iki ara\u015ft\u0131rma alan\u0131n\u0131n de\u011fi\u015fik y\u00f6ntemleri ve de\u011fi\u015fik motivasyonlar\u0131 nedeniyle yarar\u0131n yan\u0131 s\u0131ra riskler de ta\u015f\u0131yor.<\/p>\n

Karanl\u0131k \u00f6zdek ve karanl\u0131k erke<\/strong><\/p>\n

Son yirmi y\u0131lda ortaya \u00e7\u0131kan paradigma, kozmik yap\u0131lar\u0131n evrimine ili\u015fkindir. Bu paradigman\u0131n en \u00e7arp\u0131c\u0131 yan\u0131, g\u00fcn\u00fcm\u00fcz evreninin \u00f6ng\u00f6r\u00fclememi\u015f ve g\u00f6r\u00fcn\u00fcrde birbirinden ba\u011f\u0131ms\u0131z iki bile\u015fenine -karanl\u0131k erke ve karanl\u0131k \u00f6zdek<\/strong>– yap\u0131lan vurgudur. G\u00f6kada dinami\u011fini a\u00e7\u0131klayabilmek i\u00e7in g\u00f6r\u00fcnmeyen \u00f6zde\u011fe olan gereksinim ilk kez 1930 y\u0131l\u0131nda Fritz Zwicky taraf\u0131ndan ileri s\u00fcr\u00fclm\u00fc\u015ft\u00fcr. Ancak ge\u00e7en 25 y\u0131lda kozmik yap\u0131lar\u0131n b\u00fcy\u00fcmesi konusunda, yeni t\u00fcrden, zay\u0131f etkile\u015fen ve \u00e7ekimsel olarak bask\u0131n par\u00e7ac\u0131klar \u00f6n plana \u00e7\u0131km\u0131\u015ft\u0131r. Evrenimizin g\u00fcn\u00fcm\u00fczdeki ivmeli geni\u015flemesinden karanl\u0131k erkenin sorumlu oldu\u011fu g\u00f6r\u00fc\u015f\u00fc de geni\u015f bir onay g\u00f6rm\u00fc\u015ft\u00fcr; oysa ki Einstein\u2019\u0131n \u00e7ekim kuram\u0131nda sunulan kozmolojik sabit<\/strong> g\u00f6zlemlere a\u00e7\u0131klama getirebiliyor.<\/p>\n

Karanl\u0131k \u00f6zdek ve karanl\u0131k erke hem y\u00fcksek erke fizik\u00e7ileri hem de astrofizik\u00e7iler taraf\u0131ndan temel birer \u00f6\u011fe olarak g\u00f6r\u00fcl\u00fcyor. Karanl\u0131k \u00f6zdek olmaya aday t\u00fcm temel par\u00e7ac\u0131klar par\u00e7ac\u0131k fizi\u011finin yenilenip geli\u015fmesini gerektiriyor; g\u00fcn\u00fcm\u00fczde en \u00e7ok ye\u011flenen aday en hafif s\u00fcperbak\u0131\u015f\u0131k (s\u00fcpersimetrik) par\u00e7ac\u0131kt\u0131r. E\u011fer bu \u00f6ng\u00f6r\u00fc do\u011frulan\u0131rsa, erken evrenin s\u00fcperbak\u0131\u015f\u0131kl\u0131\u011f\u0131 bozacak denli s\u0131cak oldu\u011fu kan\u0131tlanacakt\u0131r. Di\u011fer yandan karanl\u0131k erke g\u00fcn\u00fcm\u00fcz par\u00e7ac\u0131k fizi\u011fi kuramlar\u0131n\u0131n k\u00f6kten de\u011fi\u015fimini dayatacakt\u0131r. Bu de\u011fi\u015fiklik, s\u00fcpersicim kuramlar\u0131n\u0131n herhangi birinde, genel g\u00f6relilik kuram\u0131yla kuantum mekani\u011finin birle\u015fmesiyle olabilecektir.<\/p>\n

Karanl\u0131k \u00f6zdek ve karanl\u0131k erkeye ili\u015fkin kan\u0131tlar tamamen g\u00f6kbilim g\u00f6zlemlerinden kaynaklan\u0131yor ve \u00f6yle g\u00f6r\u00fcn\u00fcyor ki, karanl\u0131k erkenin ge\u00e7erlilik s\u0131n\u0131rlar\u0131n\u0131 yaln\u0131zca g\u00f6kbilim g\u00f6zlemleri sa\u011flayabilecektir. K\u0131sacas\u0131, g\u00fcn\u00fcm\u00fcz y\u00fcksek erke fizi\u011fi deneylerinde en s\u0131cak g\u00fcndem olan karanl\u0131k erke, g\u00f6kbilimde yap\u0131lacak g\u00f6zlemlere ba\u011fl\u0131d\u0131r. Bu nedenle, bu sorunu ele alma konusunda her iki bilim dal\u0131 da b\u00fcy\u00fck giri\u015fimlerde bulunmak i\u00e7in i\u015fbirli\u011fi yap\u0131yor.<\/p>\n

Ancak, g\u00f6kbilim a\u00e7\u0131s\u0131ndan bakt\u0131\u011f\u0131m\u0131zda, karanl\u0131k \u00f6zdek ve karanl\u0131k erke sorunsallar\u0131 alan\u0131n di\u011fer dallar\u0131yla etkile\u015fimde farkl\u0131 niteliklere sahiptir. Karanl\u0131k \u00f6zdek g\u00f6kada k\u00fcmelerinin ve g\u00f6kadalar\u0131n olu\u015fumunu ve bu yap\u0131lar\u0131n t\u00fcm \u00f6zelliklerini belirler. Karanl\u0131k \u00f6zde\u011fin uzaydaki da\u011f\u0131l\u0131m\u0131 \u00e7ekimsel mercekleme g\u00f6zlemleriyle dolays\u0131z olarak haritalanabilir. Yine karanl\u0131k \u00f6zde\u011fe ili\u015fkin bilgiler, hem g\u00f6kada dinami\u011fi ve g\u00f6kadalararas\u0131 gaz dinami\u011fi g\u00f6zlemlerinden dolayl\u0131 olarak, hem de mikrodalga ardalan \u0131\u015f\u0131n\u0131m\u0131ndaki dalgalanmalardan derlenebilir. G\u00fcn\u00fcm\u00fczde en \u00e7ok ye\u011flenen karanl\u0131k \u00f6zdek aday\u0131, bilinen par\u00e7ac\u0131klar\u0131n en hafif s\u00fcrerbak\u0131\u015f\u0131k yolda\u015f\u0131, yok edilme \u0131\u015f\u0131n\u0131m\u0131 (annihilation radiation) \u00fcretece\u011fi i\u00e7in hen\u00fcz tasar\u0131m a\u015famas\u0131nda olan gama \u0131\u015f\u0131n teleskopuyla alg\u0131lanabilir. Karanl\u0131k \u00f6zdek yak\u0131n gelecekte yeralt\u0131 \u201cteleskoplar\u0131\u201dyla dolays\u0131z olarak alg\u0131lanabilir; yeralt\u0131 \u201cteleskoplar\u0131\u201dn\u0131n bilinen par\u00e7ac\u0131klarla karanl\u0131k \u00f6zdek par\u00e7ac\u0131klar\u0131n\u0131n zaman zaman ger\u00e7ekle\u015fen \u00e7arp\u0131\u015fmalar\u0131n\u0131 \u00f6l\u00e7me yetene\u011fi h\u0131zla geli\u015fiyor ve belki de B\u00fcy\u00fck Hadron \u00c7arp\u0131\u015ft\u0131r\u0131c\u0131s\u0131\u2019nda (Large Hadron Collider\u2019da) yap\u0131lacak deneylerde de alg\u0131lanabilir. B\u00f6ylece karanl\u0131k \u00f6zdek \u00e7al\u0131\u015fmalar\u0131, g\u00f6kada \u00f6tesi g\u00f6kbilim ve astrofiziksel kozmolojinin bir\u00e7ok dal\u0131nda oldu\u011fu gibi, astropar\u00e7ac\u0131k deneyleri ve h\u0131zland\u0131r\u0131c\u0131lardaki ara\u015ft\u0131rma programlar\u0131 i\u00e7in de olanaklar sunabilecektir.<\/p>\n

Karanl\u0131k \u00f6zde\u011fin tersine, karanl\u0131k erke \u00e7al\u0131\u015fmalar\u0131 astrofizi\u011fin ve deneysel par\u00e7ac\u0131k fizi\u011finin di\u011fer dallar\u0131na \u00e7ok az veya hi\u00e7 etkide bulunamayacakt\u0131r. Karanl\u0131k erkenin karanl\u0131k \u00f6zdek ile etkile\u015fimi sonucunda g\u00f6kada ve\/veya g\u00f6kada k\u00fcmesi gibisinden kozmik yap\u0131lar\u0131n g\u00f6zlenebilir etkilerine ili\u015fkin modeller \u00f6nerilmi\u015ftir, ancak bu modellerin \u00e7o\u011funda karanl\u0131k erke ve karanl\u0131k \u00f6zdek birbirinden ba\u011f\u0131ms\u0131zd\u0131r. Karanl\u0131k erke, etkisini yaln\u0131zca evrenin geni\u015fleme tarih\u00e7esinde ve yap\u0131lardaki d\u00fczensizliklerin do\u011frusal b\u00fcy\u00fcmesinde g\u00f6sterir. E\u011fer Einstein\u2019\u0131n \u00e7ekim kuram\u0131 do\u011fruysa, karanl\u0131k erkeye ili\u015fkin bilgiler, kozmik zaman\u0131n bir i\u015flevi olarak geni\u015fleme oran\u0131na ili\u015fkin g\u00f6kbilim g\u00f6zlemlerinden t\u00fcretilebilir.<\/p>\n

E\u011fer karanl\u0131k erke kozmolojik sabit gibi davran\u0131yorsa, elimizdeki g\u00f6kbilim verileri uzay\u0131n geni\u015fleme tarih\u00e7esiyle tutarl\u0131d\u0131r. Bu konuyla ilgili parametrenin g\u00fcn\u00fcm\u00fczdeki de\u011ferine ili\u015fkin hesaplamalar w~ – 1 \u00b1 0,1\u2019dir, burada w = – 1 t\u00fcm zamanlardaki kozmolojik sabittir. G\u00f6kbilimciler i\u00e7in bunun anlam\u0131 \u015fudur: Kozmik geni\u015fleme tarih\u00e7esi yeterince g\u00fcvenilir bir bi\u00e7imde belirlendi\u011finden bu de\u011ferin daha ayr\u0131nt\u0131l\u0131 elde edilmesi y\u00f6n\u00fcndeki \u00e7al\u0131\u015fmalar, kozmik yap\u0131lar\u0131n olu\u015fma tarih\u00e7elerine en fazla \u00e7ok k\u00fc\u00e7\u00fck bir de\u011fi\u015fiklikte bulunacakt\u0131r.<\/p>\n

K\u0131sacas\u0131, karanl\u0131k \u00f6zde\u011fin do\u011fas\u0131n\u0131n ayd\u0131nlat\u0131lmas\u0131 tipik bir astrofizik\u00e7inin sorununa damgas\u0131n\u0131 vurur ve ilgi alan\u0131n\u0131n di\u011fer yanlar\u0131yla etkile\u015fimini sa\u011flarken, karanl\u0131k erkenin do\u011fas\u0131n\u0131n belirlenmesi bir \u201ctemel\u201d sorunsald\u0131r ve bu belirlemeye giden yol astrofizi\u011fin di\u011fer alanlar\u0131na \u00e7ok az etki yapacakt\u0131r.<\/p>\n

\"\"
Hubble Uzay Teleskopu\u2019nun g\u00f6r\u00fcnt\u00fcledi\u011fi, Abell 1689 g\u00f6kada k\u00fcmesi i\u00e7inde karanl\u0131k madde haritas\u0131. Abell 1689 g\u00f6kada k\u00fcmesinin, g\u00f6zlenen k\u00fctle\u00e7ekimsel merceklenme etkisi nedeniyle, \u00f6nemli miktarda karanl\u0131k madde i\u00e7ermesi gerekti\u011fi d\u00fc\u015f\u00fcn\u00fcl\u00fcyor. (Kaynak: https:\/\/www.nasa.gov)<\/figcaption><\/figure>\n

Bunun iki sonucu olacakt\u0131r. Uzay\u0131n geni\u015fleme tarih\u00e7esindeki ve kozmik mikrodalga ardalan \u0131\u015f\u0131n\u0131m\u0131ndaki s\u0131cakl\u0131k dalgalanmalar\u0131n\u0131n daha ince ayr\u0131nt\u0131lar\u0131na ili\u015fkin \u00e7al\u0131\u015fmalar bizim, y\u0131ld\u0131zlar\u0131n, g\u00f6kadalar\u0131n ve daha b\u00fcy\u00fck \u00f6l\u00e7ekli yap\u0131lar\u0131n olu\u015fumu ve evrimi konusundaki bilgilerimizi geli\u015ftirmeyecektir. Bu bilgilerimizi g\u00fcn\u00fcm\u00fczde k\u0131s\u0131tlayan belirsizlikler, bir\u00e7ok karma\u015f\u0131k ve kar\u015f\u0131l\u0131kl\u0131 etkile\u015fim i\u00e7indeki astrofiziksel s\u00fcre\u00e7lerdir. Buna kar\u015f\u0131n, bu belirsizlikler karanl\u0131k erkenin s\u0131n\u0131rlar\u0131n\u0131 belirlemeye ili\u015fkin becerimizi art\u0131racakt\u0131r. \u00d6rne\u011fin, Ia t\u00fcr\u00fc s\u00fcpernovalar g\u00fcn\u00fcm\u00fczde kozmik geni\u015flemenin tarih\u00e7esi i\u00e7in en iyi ara\u015ft\u0131rma y\u00f6ntemidir ve planlanm\u0131\u015f programlar kullanarak, iyi g\u00f6zlenmi\u015f \u00f6rneklerin boyutlar\u0131n\u0131 ve k\u0131rm\u0131z\u0131ya kayma de\u011ferlerini, istatistiksel yan\u0131lg\u0131lar\u0131n en k\u00fc\u00e7\u00fck de\u011ferlerine dek \u00f6l\u00e7ebiliriz.<\/p>\n

Ne yaz\u0131k ki, y\u00fcksek k\u0131rm\u0131z\u0131ya kayma g\u00f6steren s\u00fcpernova atalar\u0131 daha gen\u00e7 g\u00f6kadalarda olu\u015fup patlad\u0131lar. Bu durum, s\u00fcpernovalar\u0131n veya onlar\u0131n i\u00e7inde bulundu\u011fu ortam\u0131n \u00f6zellikleri, k\u0131rm\u0131z\u0131 kaymaya ba\u011fl\u0131 de\u011fi\u015fimlerin \u00e7ok k\u00fc\u00e7\u00fck olmas\u0131na neden olur. Alg\u0131lanamayan bu de\u011fi\u015fim karanl\u0131k erke sinyali ara\u015ft\u0131rmalar\u0131nda kafa kar\u0131\u015f\u0131kl\u0131\u011f\u0131na neden olur ve \u00f6l\u00e7\u00fcmlerin do\u011frulu\u011funa s\u0131n\u0131rlamalar getirir. Buna benzer sistematik yan\u0131lg\u0131lar, \u00f6nerilen ara\u015ft\u0131rmalar\u0131 da etkiler \u00e7\u00fcnk\u00fc \u00f6l\u00e7\u00fcmler olduk\u00e7a karma\u015f\u0131k yap\u0131lara sahip g\u00f6kcisimleri ve s\u00fcpernovalar \u00fczerinde yap\u0131lmaktad\u0131r. K\u0131sacas\u0131, karanl\u0131k erke s\u0131n\u0131rlar\u0131 \u00fczerine getirilmeye \u00e7al\u0131\u015f\u0131lan daha do\u011fru s\u0131n\u0131rlamalar, evrenimizdeki g\u00f6kcisimlerinin evrimlerini anlamam\u0131za yard\u0131mc\u0131 olamayacakt\u0131r, ancak bu konudaki bilgisizli\u011fimiz de karanl\u0131k erke s\u0131n\u0131rlar\u0131na ili\u015fkin \u00e7abalar\u0131m\u0131z\u0131 k\u0131s\u0131tlayacakt\u0131r.<\/p>\n

Karanl\u0131k erke g\u00f6kbilim \u00e7al\u0131\u015fmalar\u0131 i\u00e7in neden k\u00f6t\u00fcd\u00fcr?<\/strong><\/p>\n

Astrofiziksel ara\u015ft\u0131rmalar\u0131n ba\u015fl\u0131ca g\u00fcd\u00fcc\u00fc konusu olan karanl\u0131k erke \u00fczerine yap\u0131lan vurgu, yaln\u0131zca astrofizi\u011fin y\u00f6ntemsel temelini de\u011fil, ayn\u0131 zamanda bu konular\u0131n \u00e7ekicili\u011fini, gelecek nesillerin en yetenekli astrofizik\u00e7ilerini ve kamuyu olumsuz etkileyecektir. B\u00f6ylesi olumsuz sonu\u00e7lar astrofizi\u011fe yabanc\u0131 olan y\u00fcksek erke fizi\u011fi k\u00fclt\u00fcr\u00fcn\u00fcn astrofizi\u011fe bula\u015fmas\u0131 ve \u00f6zellikle de g\u00f6kbilimi etkileyen ba\u011f\u0131ms\u0131z bir e\u011filim olan \u201cb\u00fcy\u00fck bilim\u201d ile birlikte gelerek olacakt\u0131r.<\/p>\n

Bu konuda \u00fc\u00e7 t\u00fcr \u00e7ekince bulunuyor: B\u00fcy\u00fck programlar\u0131n tasar\u0131m\u0131nda risk de\u011ferlendirmesi uygun olmayacakt\u0131r; s\u0131n\u0131rl\u0131 kaynaklar astrofizikte yeni alanlar a\u00e7amayacak ve daha geni\u015f ara\u015ft\u0131rma alanlar\u0131 y\u00fcceltemeyecektir; ve \u201ctemel de\u011ferler\u201d dizgesini y\u00fcceltmek, g\u00f6kbilimin, parlak, \u00e7ok yarat\u0131c\u0131, en tutkulu ve istekli gen\u00e7 biliminsanlar\u0131n\u0131n g\u00f6z\u00fcnde \u00e7ekicili\u011fini yitirmesine neden olacakt\u0131r.<\/p>\n

Son zamanlarda mikrodalga ardalan \u0131\u015f\u0131n\u0131m\u0131 \u00e7al\u0131\u015fmalar\u0131ndaki ola\u011fan\u00fcst\u00fc ilerleme, bir\u00e7ok ki\u015fiyi, astrofiziksel kozmolojinin temel fizikte yeni bir pencere a\u00e7t\u0131\u011f\u0131na inand\u0131rd\u0131. Bu ilerlemeler olas\u0131yd\u0131; \u00e7\u00fcnk\u00fc g\u00f6zlenen \u0131\u015f\u0131n\u0131m, basit bir durumda do\u011frusal tedirginlikler sergiliyor. Bu \u0131\u015f\u0131n\u0131m\u0131n evrimi \u00fczerinde inceden inceye ve do\u011fru bir bi\u00e7imde \u00e7al\u0131\u015fma yap\u0131labilir.<\/p>\n

Buna ek olarak, mikrodalga ardalan \u0131\u015f\u0131n\u0131m\u0131 \u00fczerine \u00f6n alan\u0131n etkileri olduk\u00e7a zay\u0131ft\u0131r ve \u00e7ok k\u00fc\u00e7\u00fck karma\u015f\u0131kl\u0131\u011fa neden olacak cinstendir. Ardalan \u0131\u015f\u0131n\u0131m\u0131 \u00fczerine elde edilen bu ba\u015far\u0131yla evrenbilime y\u00f6nelmi\u015f olan \u201ck\u00f6kten fizik\u00e7iler\u201d (fundamentalist physicists) \u00e7o\u011fu zaman ko\u015fullar\u0131n \u00f6zg\u00fcnl\u00fc\u011f\u00fcn\u00fc kavramakta yetersiz kal\u0131yor. Bu ba\u011flamda helyosismolojiyle mikrodalga ardalan \u0131\u015f\u0131n\u0131m\u0131 aras\u0131nda bir kar\u015f\u0131la\u015ft\u0131rma yapabiliriz. G\u00fcne\u015f\u2019in yap\u0131s\u0131 \u00fczerine yap\u0131lan \u00e7al\u0131\u015fmalar G\u00fcne\u015f\u2019ten kaynaklanan ses dalgalar\u0131n\u0131n yay\u0131lmas\u0131 g\u00f6zlemiyle yap\u0131l\u0131r. G\u00fcne\u015f\u2019te ses dalgalar\u0131n\u0131n \u00fcretilmesine neden olan tedirginlikler de do\u011frusald\u0131r ve yay\u0131ld\u0131klar\u0131 ortam\u0131n fizi\u011fi de \u00e7ok iyi anla\u015f\u0131lm\u0131\u015ft\u0131r. Bu alanda ger\u00e7ekle\u015ftirilmi\u015f olan dikkatli \u00f6l\u00e7\u00fcmler, \u00e7ok say\u0131daki dalga bi\u00e7emleriyle (wave modes) ilgili son derece do\u011fru sonu\u00e7lar vermi\u015ftir. Ancak kozmik mikrodalga ardalan \u0131\u015f\u0131n\u0131m\u0131 \u00e7al\u0131\u015fmalar\u0131ndan elde edilen, istatistiksel g\u00fcvenirli\u011fine ve do\u011frulu\u011funa ili\u015fkin sonu\u00e7lar, \u0131\u015f\u0131n\u0131m\u0131 olu\u015fturan altyap\u0131n\u0131n karma\u015f\u0131k olmas\u0131 nedeniyle ku\u015fku do\u011fmas\u0131na neden oluyor. \u00d6rne\u011fin, g\u00fcne\u015f evrimine ili\u015fkin standart modellerin, helyosismolojinin sonu\u00e7lar\u0131na uygun gelebilmesi i\u00e7in gereksinim duydu\u011fu ba\u015flang\u0131\u00e7 a\u011f\u0131r elementler niceli\u011fi, G\u00fcne\u015f atmosferinden tayf analiziyle elde edilen niceli\u011fin hemen hemen iki kat\u0131d\u0131r.<\/p>\n

\"\"
Karanl\u0131k maddenin sanatsal bir temsili. (http:\/\/www.zmescience.com\/space\/astrophysics-space\/dark-energy-dark-matter-11032014\/)<\/figcaption><\/figure>\n

Karanl\u0131k erkenin astrofiziksel a\u00e7\u0131dan anla\u015f\u0131lmas\u0131n\u0131n en iyi yollar\u0131 karma\u015f\u0131k dizgelerden ge\u00e7er: Evrenin geni\u015fleme tarih\u00e7esini izlemek i\u00e7in s\u00fcpernovalar; \u00f6zde\u011fin b\u00fcy\u00fck \u00f6l\u00e7eklerde da\u011f\u0131l\u0131m\u0131ndaki dalgalanmalar\u0131 \u00f6zetlemek i\u00e7in g\u00f6kadalar; \u00f6nalandaki k\u00fctle da\u011f\u0131l\u0131m\u0131n\u0131n neden oldu\u011fu \u00e7ekimsel merceklemenin izini s\u00fcrmek i\u00e7in ardalan kaynaklar\u0131 olarak g\u00f6kadalar ve kozmik yap\u0131lar\u0131n b\u00fcy\u00fcmesinin i\u015faret\u00e7ileri olarak g\u00f6kada k\u00fcmeleri. Astrofizikte kazan\u0131lan deneyimler bu t\u00fcr programlar\u0131n son ba\u015far\u0131s\u0131n\u0131n sistematik etkilerle belirlenece\u011fine i\u015faret ediyor; \u00f6rne\u011fin, s\u00fcpernovalar ba\u011flam\u0131nda ata y\u0131ld\u0131z\u0131n ve \u00e7evresindeki ortam\u0131n evrimi; g\u00f6kadalar ve g\u00f6kada k\u00fcmelerine ili\u015fkin g\u00f6zlemler ve kuramsal nicelikler aras\u0131ndaki do\u011frusal olmayan ve belirlenemez ili\u015fkiler. Bu t\u00fcr sistematik \u00e7al\u0131\u015fmalar do\u011fas\u0131 gere\u011fi \u00f6nceden de\u011ferlendirilemez ve program tamamlan\u0131ncaya dek tan\u0131s\u0131 yap\u0131lmam\u0131\u015f olarak kal\u0131rlar.<\/p>\n

Karanl\u0131k erke deneylerinin do\u011frulu\u011funa ili\u015fkin son de\u011ferlendirmeler tamamen istatistiksel \u00e7al\u0131\u015fmalar temelinde yap\u0131l\u0131r ve \u201cen olas\u0131\u201d sonu\u00e7, en iyimser de\u011ferlendirme olarak sunulur. Karanl\u0131k erke hayranlar\u0131 kozmik ardalan \u0131\u015f\u0131n\u0131m\u0131<\/strong> \u00e7al\u0131\u015fmalar\u0131ndaki ba\u015far\u0131lardan y\u00fcreklendirildi ve \u00e7o\u011fu zaman s\u0131n\u0131rlamalar\u0131n ay\u0131rt\u0131na varamad\u0131lar, sofistike istatistiksel \u00e7al\u0131\u015fmalar\u0131n en olas\u0131 sonucu verece\u011fini sand\u0131lar. Bu durum ara\u015ft\u0131rma alan\u0131n\u0131 binlerce s\u00fcpernova \u00f6l\u00e7me veya uzay\u0131n \u00e7ok b\u00fcy\u00fck bir b\u00f6l\u00fcm\u00fcn\u00fcn g\u00f6r\u00fcnt\u00fcs\u00fcn\u00fc \u00e7\u0131karma gibi \u00e7ok pahal\u0131 deneyler tasarlay\u0131p yap\u0131p \u00f6l\u00e7me \u00e7ekincesiyle kar\u015f\u0131 kar\u015f\u0131ya b\u0131\u0131rak\u0131r. Sonu\u00e7ta w \u00f6l\u00e7\u00fcm sonu\u00e7lar\u0131n\u0131n \u00f6nceki \u00e7al\u0131\u015fma sonu\u00e7lar\u0131ndan biraz daha iyi oldu\u011fu bulunur. E\u011fer yap\u0131lan deney, di\u011fer astrofiziksel ama\u00e7lar i\u00e7in kullan\u0131\u015fs\u0131z olacaksa, elde edilen parasal destekler harcanm\u0131\u015f olacakt\u0131r. Bu da kesinlikle astrofizik\u00e7ilerin su\u00e7lanmas\u0131na neden olur!<\/p>\n

\u0130kinci \u00e7ekince, karanl\u0131k erkeye yap\u0131lan bu yo\u011fun vurgu, astrofizikte bir sonraki a\u015faman\u0131n olanaklar\u0131n\u0131 planlarken, astrofizi\u011fin g\u00fcc\u00fcn\u00fc yitirmesine neden olacakt\u0131r. G\u00f6kbilimciler duyarl\u0131l\u0131k, dalgaboyu aral\u0131\u011f\u0131, uzay ve renk \u00e7\u00f6z\u00fcn\u00fcrl\u00fc\u011f\u00fc gibi teknik yeteneklere yo\u011funla\u015f\u0131p yeni alga\u00e7lar tasarlarken, geleneksel olarak ortaya \u00e7\u0131kacak riski en aza indirmeye \u00e7al\u0131\u015f\u0131rlar. Bu yakla\u015f\u0131m \u00e7ok geni\u015f sorunsallar\u0131n \u00e7\u00f6z\u00fcm\u00fc konusunda ilerleme sa\u011flar, \u00f6zellikle de g\u00f6zlemevi temelinde yap\u0131lan \u00e7al\u0131\u015fmalar, ilgin\u00e7 oldu\u011funa inan\u0131lan yeni projelerin sunulmas\u0131n\u0131 sa\u011flar.<\/p>\n

Baz\u0131 karanl\u0131k erke projeleri bu amaca uygundur. \u00d6rne\u011fin, geni\u015f \u2013 alan X \u2013 \u0131\u015f\u0131n ve milimetre dalgaboyunda yap\u0131lacak olan g\u00f6ky\u00fcz\u00fc taramalar\u0131 \u00e7ok say\u0131da uzak g\u00f6kada k\u00fcmelerinin tan\u0131s\u0131ndan ba\u015fka, uzay\u0131n geni\u015f bir b\u00f6lgesini ilgili dalgaboylar\u0131nda daha \u00f6nce ula\u015f\u0131lmam\u0131\u015f olan duyarl\u0131kta ve \u00e7\u00f6z\u00fcn\u00fcrl\u00fckte g\u00f6r\u00fcnt\u00fcleyecektir. Bu olanaklar, s\u0131n\u0131rl\u0131 da olsa g\u00f6zlemevlerinde ger\u00e7ekle\u015fecektir. Di\u011fer karanl\u0131k erke projeleri, \u00f6rne\u011fin, s\u00fcpernovalar\u0131 ara\u015ft\u0131ran veya b\u00fcy\u00fck \u00f6l\u00e7ekte g\u00f6kada ve k\u00fctle da\u011f\u0131l\u0131m\u0131 \u00f6l\u00e7\u00fcmlerinde baryonik \u00f6zdek ara\u015ft\u0131rmalar\u0131 bu konularda elde edilen duyarl\u0131l\u0131kta, \u00e7\u00f6z\u00fcn\u00fcrl\u00fckte veya dalgaboyu aral\u0131klar\u0131nda bir geli\u015fme g\u00f6stermeyecektir.<\/p>\n

Bu t\u00fcr ara\u015ft\u0131rmalar astrofizi\u011fin di\u011fer alanlar\u0131nda geli\u015fmelere neden olamayacakt\u0131r. \u00d6rne\u011fin g\u00f6ky\u00fcz\u00fcn\u00fcn iki kare derecelik b\u00f6lgesinin derin fotometrik g\u00f6r\u00fcnt\u00fcs\u00fc zaten yap\u0131ld\u0131 ve y\u00fcz binlerce s\u00f6n\u00fck g\u00f6kadaya ili\u015fkin verileri toplad\u0131. G\u00f6kada olu\u015fumu ve evrimine ili\u015fkin yaln\u0131zca birka\u00e7 \u00e7al\u0131\u015fma, karanl\u0131k erke projesinin sa\u011flad\u0131\u011f\u0131 \u00f6rneklere benzer ancak 1000 kez daha fazla veriden yararlanacakt\u0131r. Varolan alga\u00e7lar\u0131n duyarl\u0131l\u0131\u011f\u0131 bu projelerin yetene\u011fi d\u00fczeyinde oldu\u011fu i\u00e7in, projelerin g\u00f6zlemevi bi\u00e7eminde uygulanmas\u0131 te\u015fvik edici nitelikte olmayacakt\u0131r.<\/p>\n

Burada astrofizik \u00e7al\u0131\u015fmalar\u0131 i\u00e7in ortaya \u00e7\u0131kan \u00e7ekince \u015fudur: G\u00f6kbilimcilerle par\u00e7ac\u0131k fizik\u00e7ilerinin yak\u0131nla\u015fmas\u0131 karanl\u0131k erke deneyleri yarar\u0131na g\u00fc\u00e7l\u00fc bir lobi olu\u015fturacakt\u0131r. \u00d6nerilen b\u00fcy\u00fck projeler aras\u0131ndaki do\u011fal rekabette bu t\u00fcr bir lobi X-\u0131\u015f\u0131n, radyo, mor\u00f6te ve k\u0131z\u0131l\u00f6te dalgaboylar\u0131nda g\u00f6zlem yapan geleneksel g\u00f6zlemevlerinin zarar\u0131na olacakt\u0131r. G\u00f6kbilimciler, onlar\u0131n temel ara\u015ft\u0131rma alanlar\u0131na \u00e7ok az etkisi olacak olan deneylerle zamanlar\u0131n\u0131, erkelerini ve kaynaklar\u0131n\u0131 yitirecekler, bu arada, onlar\u0131 geleneksel olarak yarat\u0131c\u0131l\u0131\u011fa, yenili\u011fe ve alanlar\u0131nda bilgi art\u0131r\u0131m\u0131na s\u00fcren olanaklar\u0131 feda etmelerine neden olacakt\u0131r.<\/p>\n

Karanl\u0131k erke ortak projelerinin \u00fc\u00e7\u00fcnc\u00fc ve en ciddi \u00e7ekincesi \u015fudur: K\u00f6ktenci y\u00fcksek erke par\u00e7ac\u0131k fizik\u00e7ilerinin, \u201cKaranl\u0131k erke do\u011fas\u0131n\u0131n a\u00e7\u0131kl\u0131\u011fa \u00e7\u0131kar\u0131lmas\u0131 g\u00fcn\u00fcm\u00fcz astrofizi\u011finin en acil sorunudur\u201d g\u00f6r\u00fc\u015f\u00fcn\u00fc onarlarsa, astrofizik\u00e7iler kendi k\u00fclt\u00fcr dokular\u0131n\u0131n temelini arkadan vururlar, astrofizi\u011fin, gelecek nesillerin yarat\u0131c\u0131 biliminsanlar\u0131na ve geni\u015f \u00f6l\u00e7\u00fcde kamuya olan \u00e7ekicili\u011fini yok ederler.<\/p>\n

\u015eekil 1\u2019de NASA\u2019n\u0131n Astrofizik Veri Taban\u0131ndan (ADS) derlenmi\u015f olan bir bibliyografik istatistik g\u00f6sterilmi\u015ftir. Bu istatistikte son 30 y\u0131lda astrofizikteki ve uzay bilimlerindeki de\u011fi\u015fiklikler g\u00f6sterilmi\u015ftir. 1975 y\u0131l\u0131nda yakla\u015f\u0131k 8500 yazar hakemli dergilerde toplam 8900 makale yay\u0131mlatm\u0131\u015ft\u0131r. 2006 y\u0131l\u0131nda yazar say\u0131s\u0131 d\u00f6rde katlanm\u0131\u015f, ancak makale say\u0131s\u0131 yaln\u0131zca iki kat artm\u0131\u015ft\u0131r. G\u00f6kbilim toplulu\u011funun \u00fcye say\u0131s\u0131 b\u00fcy\u00fck \u00f6l\u00e7\u00fcde artm\u0131\u015f, \u00fcyelerin \u00fcretkenli\u011findeki azal\u0131\u015f, yay\u0131mlanan her bir makaleye daha fazla bireyin ad\u0131n\u0131n yaz\u0131lmas\u0131yla maskelenmi\u015ftir. 1975 y\u0131l\u0131nda birinci s\u0131n\u0131f dergilerde yay\u0131mlanan t\u00fcm makalelerin y\u00fczde 40\u2019\u0131ndan fazlas\u0131 bir yazarl\u0131 ve y\u00fczde 3\u2019\u00fcnden az\u0131 6 veya daha fazla yazarl\u0131yd\u0131.2006 y\u0131l\u0131nda yay\u0131mlanan makalelerin yaln\u0131zca y\u00fczde \u00a09\u2019u tek yazarl\u0131 ve y\u00fczde 28\u2019i 6 veya daha fazla yazarl\u0131d\u0131r.<\/p>\n

\"\"
Smitsonian\/NASA Astrophysical Data System verileriyle olu\u015fturulan yay\u0131n istatisti\u011fi. \u015eekil 1975-2006 d\u00f6neminde astrofizik etkinliklerinin artt\u0131\u011f\u0131n\u0131 g\u00f6steriyor. S\u00fcrekli siyah \u00e7izgi hakemli dergilerde yay\u0131nlanan astrofizik makalelerinin y\u0131ll\u0131k say\u0131s\u0131n\u0131 g\u00f6steriyor. Uzun kesikli ye\u015fil \u00e7izgi bu makalelerin ayr\u0131 ayr\u0131 yazarlar\u0131na i\u015faret ediyor. Noktal\u0131-kesikli mavi \u00e7izgi makalede ad\u0131 ge\u00e7en yazarlar\u0131n ortalama say\u0131s\u0131n\u0131 g\u00f6steriyor. K\u0131sa kesikli k\u0131rm\u0131z\u0131 \u00e7izgi her bir makalenin referans listesine giri\u015f ortalama say\u0131s\u0131n\u0131 g\u00f6steriyor. T\u00fcm istatistikler 1975 y\u0131l\u0131nda birim de\u011fere normalize edilmi\u015ftir. 1975 y\u0131l\u0131na ait ger\u00e7ek de\u011ferler parantez i\u00e7inde g\u00f6sterilmi\u015ftir.1975 y\u0131l\u0131ndan 2006 y\u0131l\u0131na dek olan s\u00fcrede etkin olarak \u00e7al\u0131\u015fan astrofizik\u00e7ilerin say\u0131s\u0131 d\u00f6rt kat artm\u0131\u015ft\u0131r. Hakemli dergi makaleleri ve her bir makaledeki yazar say\u0131s\u0131 iki kattan fazla artm\u0131\u015ft\u0131r.<\/figcaption><\/figure>\n

Bireysel \u00e7al\u0131\u015fmalar yerine grup \u00e7al\u0131\u015fmalar\u0131na do\u011fru bir e\u011filimin oldu\u011fu kesin, ancak burada \u00e7al\u0131\u015fman\u0131n \u00f6l\u00e7\u00fct\u00fc olarak al\u0131nan at\u0131flar \u00f6ne \u00e7\u0131kar\u0131l\u0131yor. Bu uygulama da, \u015eekil 1\u2019de g\u00f6r\u00fclece\u011fi gibi bir ba\u015fka e\u011filimi g\u00fc\u00e7lendiriyor: hakemli astrofizik makalelerinin referans listesi 1975-2006 d\u00f6neminde ortalama 3,4 kat artm\u0131\u015ft\u0131r. Bir yazar\u0131n belli bir y\u0131lda ald\u0131\u011f\u0131 at\u0131f say\u0131s\u0131, makale say\u0131s\u0131, yazar\u0131n referans listesinin uzunlu\u011fu, at\u0131f alan makaledeki yazar say\u0131s\u0131 \u00e7arp\u0131m\u0131yla belirlendi\u011fi i\u00e7in 2006 y\u0131l\u0131nda at\u0131f almak 1975 y\u0131l\u0131nda hatta 1995 y\u0131l\u0131nda at\u0131f almaktan daha kolayd\u0131r.<\/p>\n

U\u00e7 bir \u00f6rnek olarak, makalelere yap\u0131lan at\u0131f baz\u0131nda d\u00f6rd\u00fcnc\u00fc s\u0131n\u0131f bir astrofizik\u00e7inin, ge\u00e7ti\u011fimiz son on y\u0131lda, hakemli dergilerde isminin birinci s\u0131rada yer ald\u0131\u011f\u0131 bir makalesi yoktur; ald\u0131\u011f\u0131 at\u0131flar, grup \u00e7al\u0131\u015fmas\u0131nda tamamen i\u015flevsel rol\u00fc oldu\u011funa ili\u015fkin imzalad\u0131\u011f\u0131 resmi belgeler nedeniyledir. Say\u0131s\u0131 giderek artan bu ortak \u00e7al\u0131\u015fmalar daha fazla astrofizik\u00e7inin y\u00f6nlendirilmi\u015f, yar\u0131 i\u015flevsel rol\u00fc oldu\u011funa ve \u00e7ok az\u0131n\u0131n ger\u00e7ekten yarat\u0131c\u0131 bilim yapt\u0131\u011f\u0131na i\u015faret eder.<\/p>\n

B\u00fcy\u00fck ve uzun erimli projeler \u00fczerine yo\u011funla\u015fma par\u00e7ac\u0131k h\u0131zland\u0131r\u0131c\u0131lar\u0131n\u0131 kullanan fizikte bask\u0131n duruma gelmi\u015ftir. Karanl\u0131k erke projeleri astrofizikte de bu e\u011filimi ivmelendirecektir. Yaln\u0131zca b\u00fcy\u00fck g\u00f6ky\u00fcz\u00fc taramalar\u0131 kozmik geni\u015fleme ve yap\u0131lar\u0131n b\u00fcy\u00fcme tarih\u00e7esinin y\u00fczde 1 oran\u0131nda ilerletme beklentisi var. Bu birincil g\u00f6ky\u00fcz\u00fc taramalar\u0131n\u0131n ba\u015far\u0131s\u0131n\u0131n karanl\u0131k erke sorunsal\u0131n\u0131n \u00f6tesinde astrofizi\u011fe etkisi \u00e7ok az olacakt\u0131r. Bu g\u00f6ky\u00fcz\u00fc taramalar\u0131nda ara\u015ft\u0131rmac\u0131lar\u0131n \u00e7o\u011fu veri kalitesi ve projenin zaman\u0131nda bitirilmesi gibi i\u015flevsel g\u00f6revlere yo\u011funla\u015facakt\u0131r. Bu durumu, bireylerin veya k\u00fc\u00e7\u00fck gruplar\u0131n yeni fikirler geli\u015ftirip yeni alga\u00e7lar yapt\u0131\u011f\u0131 durumla kar\u015f\u0131la\u015ft\u0131r\u0131rsak, geleneksel g\u00f6kbilim ara\u015ft\u0131rmalar\u0131n\u0131n bilimsel kazan\u0131mlar\u0131n\u0131n daha b\u00fcy\u00fck oldu\u011fu g\u00f6r\u00fcl\u00fcr.<\/p>\n

\u0130leri g\u00f6r\u00fc\u015fl\u00fc g\u00f6zlemevi geli\u015ftirme program\u0131 daima yeni sorunsallar\u0131n varl\u0131\u011f\u0131n\u0131 ve bilimsel cepheyi geni\u015fletme olanaklar\u0131n\u0131 garantiler. Bu gen\u00e7 ara\u015ft\u0131rmac\u0131lar i\u00e7in \u00e7ekici bir modeldir. Yani mezun olan \u00f6\u011frenciler bilimsel katk\u0131larda bulunabilir, uluslararas\u0131 ve heyecan verici alanlarda kendilerini kan\u0131tlay\u0131p ba\u011f\u0131ms\u0131z ara\u015ft\u0131rmac\u0131lar olabilir. B\u00fcy\u00fck g\u00f6ky\u00fcz\u00fc tarama projelerinde, \u00f6zellikle de karanl\u0131k erke ara\u015ft\u0131rmalar\u0131nda bu t\u00fcr olanaklar \u00e7ok enderdir.<\/p>\n

Astrofiziksel ara\u015ft\u0131rmalar\u0131n \u00f6n\u00fcndeki \u00fc\u00e7\u00fcnc\u00fc sorun da budur. E\u011fer karanl\u0131k erke s\u0131n\u0131rlar\u0131n\u0131 belirleme amac\u0131yla yap\u0131lacak olan \u00e7ok b\u00fcy\u00fck g\u00f6ky\u00fcz\u00fc tarama projeleri g\u00f6kbilim projelerine bask\u0131n gelirse, astrofiziksel yeni geli\u015fmelerde yava\u015flama olacak ve yarat\u0131c\u0131 bireysel ara\u015ft\u0131rma alanlar\u0131 k\u0131s\u0131tlanacakt\u0131r. Bu durum, ilgi alan\u0131m\u0131z\u0131n bir\u00e7ok istekli gen\u00e7 biliminsanlar\u0131na daha az \u00e7ekici olmas\u0131na, ilgilerinin biyofizik veya nanoteknoloji gibi di\u011fer alanlara kaymas\u0131na neden olacakt\u0131r. \u0130lginin geleneksel \u00e7ok \u00e7e\u015fitli alanlar yerine bir tek \u201ctemel\u201d sorunsala yo\u011funla\u015fmas\u0131, g\u00f6kbilimin kamudaki ilgisini de k\u00f6reltecek, bilimsel \u00e7al\u0131\u015fmalar\u0131m\u0131z i\u00e7in gerekli pahal\u0131 ayg\u0131t, alga\u00e7, vb. i\u00e7in vergi m\u00fckelleflerinden gelecek deste\u011fi azaltacakt\u0131r. Karanl\u0131k erke \u201cfareli k\u00f6y\u00fcn kavalc\u0131s\u0131n\u0131n kaval\u0131d\u0131r\u201d, g\u00f6kbilimcileri parlak vaatlerle kendi ilgi alanlar\u0131ndan uzakla\u015ft\u0131r\u0131p par\u00e7ac\u0131k fizi\u011fi alan\u0131na kaymalar\u0131na ve orada da mesleklerini yitirmelerine neden olacakt\u0131r.<\/p>\n

Ne yapmal\u0131?<\/strong><\/p>\n

Yukar\u0131da \u00f6zetlenen olumsuz sonu\u00e7lar bug\u00fcnk\u00fc konumumuzdan kaynaklanacak anlam\u0131na gelmiyor. Benim bu makaledeki amac\u0131m, g\u00f6kbilimcilerin dikkatini onlar\u0131 bekleyen \u00e7ekinceye yo\u011funla\u015ft\u0131rmakt\u0131r. E\u011fer g\u00f6kbilimciler, ele\u015ftirel yakla\u015f\u0131mlar\u0131n\u0131 terk edip, s\u0131rf par\u00e7ac\u0131k fizik\u00e7ileri karanl\u0131k erkenin do\u011fas\u0131n\u0131 a\u00e7\u0131kl\u0131\u011fa kavu\u015fturmay\u0131 \u201ctemel\u201d bir sorunsal olarak g\u00f6rd\u00fc\u011f\u00fc i\u00e7in, \u00e7abalar\u0131n\u0131 ve kaynaklar\u0131n\u0131 o y\u00f6ne ak\u0131t\u0131rlarsa, b\u00fcy\u00fck bir \u00e7ekinceyle kar\u015f\u0131 kar\u015f\u0131ya kal\u0131rlar. Bu konuda \u201cmaliyet-yarar\u201d analizini ince eleyip s\u0131k dokumalar\u0131 gerekiyor. G\u00f6zlemsel astrofizi\u011fin do\u011fal s\u0131n\u0131rlar\u0131n\u0131n ve g\u00f6kbilim toplulu\u011fuyla par\u00e7ac\u0131k fizi\u011fi toplulu\u011funun k\u00fclt\u00fcrel farkl\u0131l\u0131klar\u0131n\u0131n ay\u0131rt\u0131na varmam\u0131z gerekiyor.<\/p>\n

Karanl\u0131k erke yaln\u0131zca g\u00f6kbilim g\u00f6zlemleriyle ara\u015ft\u0131r\u0131labilecek derin ve ilgin\u00e7 bir sorunsald\u0131r. Ancak bu sorunsal bir\u00e7ok ilgin\u00e7 sorunsaldan yaln\u0131zca bir tanesidir ve \u201c\u00e7\u00f6z\u00fcm\u00fc\u201d \u00e7ok d\u00fc\u015f\u00fck olas\u0131l\u0131kla yap\u0131labilecek bir sorunsald\u0131r. G\u00f6kbilimcilerin beklenen duyarl\u0131kta g\u00f6zlem yap\u0131p yapamayacaklar\u0131n\u0131 bilemiyorum, yapabilecek olsalar da, y\u00fcksek erke kuramc\u0131lar\u0131 uzay\u0131n g\u00f6zlenen geni\u015flemesi ve b\u00fcy\u00fck \u00f6l\u00e7ekli yap\u0131lar\u0131n b\u00fcy\u00fcme tarih\u00e7esiyle uyumlu bir\u00e7ok model geli\u015ftirebilecektir. Karanl\u0131k erkenin s\u0131n\u0131rlar\u0131 belirlenebilir, bu konudaki olas\u0131l\u0131klar\u0131n \u00e7o\u011fu d\u0131\u015flanabilir, ancak bir\u00e7o\u011fu da varl\u0131\u011f\u0131n\u0131 s\u00fcrd\u00fcrecektir. G\u00f6kbilimciler bu konuda uyan\u0131k olmal\u0131d\u0131r ve karanl\u0131k erke projelerine olan gereksinimle astrofizi\u011fin temel sorunsallar\u0131na ili\u015fkin projeler aras\u0131nda bir denge kurmal\u0131d\u0131r. Astrofizi\u011fin ilgi alanlar\u0131ndan vazge\u00e7ip karanl\u0131k erkenin temel do\u011fas\u0131 sorunsal\u0131yla kand\u0131r\u0131lmamal\u0131y\u0131z.<\/p>\n

Temel fizik\u00e7ilerin, \u201ckaranl\u0131k erke g\u00f6kbilim \u00e7al\u0131\u015fmalar\u0131n\u0131n ba\u015fl\u0131ca sorunsal\u0131 olmal\u0131\u201d g\u00f6r\u00fc\u015f\u00fcn\u00fc onamadan karanl\u0131k erkeyi g\u00f6kbilimsel \u00e7al\u0131\u015fmalar\u0131n temel sorunu olarak onamak i\u00e7in a\u015fa\u011f\u0131daki \u00f6nerileri sunuyorum:<\/p>\n

1) Astrofizik\u00e7iler kendi alanlar\u0131n\u0131n ve y\u00fcksek erke fizik\u00e7ilerinin k\u00fclt\u00fcrleri aras\u0131ndaki fark\u0131n ay\u0131rt\u0131nda olmal\u0131d\u0131r. Astrofizik\u00e7iler g\u00f6kbilimdeki bulgular konusunda tart\u0131\u015fmaya istekli olmal\u0131d\u0131rlar \u2013 evrenin geni\u015flemesi, kimyasal elementlerin y\u0131ld\u0131zlarda olu\u015fmas\u0131, karadeliklerin varl\u0131\u011f\u0131 ve G\u00fcne\u015f\u2019ten daha k\u00fctleli olduklar\u0131, g\u00f6kadalar\u0131n s\u00fcrekli olarak bi\u00e7im de\u011fi\u015ftirdikleri, ba\u015fka y\u0131ld\u0131zlar\u0131n \u00e7evresinde ba\u015fka gezegenlerin doland\u0131\u011f\u0131. G\u00f6kbilimciler, uzay zaman ve \u00f6zde\u011fin yap\u0131s\u0131n\u0131n ara\u015ft\u0131r\u0131lmas\u0131n\u0131n daha derin ve daha temel sorunlar oldu\u011funa, bu nedenle fiziksel d\u00fcnyaya ili\u015fkin bilgilerimizin geni\u015flemesi \u00e7abas\u0131nda entelekt\u00fcel \u00f6ncelik verilmesine ili\u015fkin par\u00e7ac\u0131k fizik\u00e7ilerin \u201ctemel\u201d savlar\u0131na kar\u015f\u0131 direnmelidir.<\/p>\n

2) B\u00fcy\u00fck g\u00f6kbilim projeleri, karanl\u0131k erke sorunsal\u0131n\u0131 temel g\u00fcd\u00fcc\u00fc olarak alan projeler de dahil olmak \u00fczere, astrofizi\u011fin \u00e7evrenini (ufkunu) geni\u015fletecek bi\u00e7imde tasarlanmal\u0131d\u0131r. S\u00fcpernova ara\u015ft\u0131rmalar\u0131, evrenin geni\u015fleme tarih\u00e7esinin izini s\u00fcrmenin yan\u0131 s\u0131ra, s\u00fcpernovalar\u0131n evrim s\u00fcrecini ve geli\u015ftikleri ortamdaki y\u0131ld\u0131zlar toplulu\u011fuyla olan ili\u015fkilerini ayd\u0131nlatacak yeterli nicelikte bilgi toplamal\u0131d\u0131r. G\u00f6kada k\u0131rm\u0131z\u0131ya kaymalar\u0131 ile ilgili ara\u015ft\u0131rmalar, iyi tan\u0131mlanm\u0131\u015f g\u00f6kadalar\u0131n nitelikli tayflar\u0131n\u0131 elde etmelidir ki g\u00f6kada evrimleri \u00fczerine kaliteli ara\u015ft\u0131rmalar yap\u0131labilsin. Ayr\u0131ca, g\u00f6kada k\u00fcmelerinin standart uzakl\u0131k \u00f6l\u00e7e\u011fi olarak kullan\u0131labilmeleri i\u00e7in uzaysal boyutlar\u0131n\u0131n \u00f6l\u00e7\u00fclmesi gerekir.<\/p>\n

3) Projelerin \u00f6nceli\u011fi, ilgi alan\u0131n\u0131n amac\u0131na g\u00f6re de\u011fil, bir b\u00fct\u00fcn olarak astrofizi\u011fin gelecekteki ilerlemesini sa\u011flayacak bi\u00e7imde olmal\u0131d\u0131r. Karanl\u0131k erke ara\u015ft\u0131rmalar\u0131 ba\u011flam\u0131nda bunun anlam\u0131 \u015fudur: Kozmik geni\u015fleme ve yap\u0131lar\u0131n b\u00fcy\u00fcmesindeki do\u011frusal dalgalanmalar gibisinden temel niceliklerin \u00f6l\u00e7\u00fcmlerindeki iyile\u015ftirmelerin, fiziksel kozmolojinin di\u011fer alanlar\u0131na \u00f6nemli katk\u0131da bulunma olas\u0131l\u0131\u011f\u0131 olduk\u00e7a d\u00fc\u015f\u00fckt\u00fcr.<\/p>\n

4) B\u00fcy\u00fck projelerin \u00e7ok say\u0131da ara\u015ft\u0131rmac\u0131ya ve uzun zaman dilimlerine gereksinimi vard\u0131r. Bu durum gen\u00e7 biliminsanlar\u0131n\u0131n yarat\u0131c\u0131l\u0131k \u015fans\u0131 \u00fczerine olumsuz etki yapacakt\u0131r. Ara\u015ft\u0131rma grubunda gen\u00e7 biliminsanlar\u0131n\u0131 bekleyen bu olumsuzlu\u011fun ortadan kald\u0131r\u0131lmas\u0131 i\u00e7in \u00e7ok \u00e7e\u015fitli bilimsel ama\u00e7lar\u0131n y\u00fcceltilmesi gerekir. Uzay\u0131n 2 a\u00e7\u0131 derecelik b\u00f6lgesinde g\u00f6kada k\u0131rm\u0131z\u0131ya kayma ara\u015ft\u0131rmas\u0131 (Two Degree Field Galaxy Redshift Survey \u2013 2dFGRS) ve Sloan Dijital Uzay Taramas\u0131 (Sloan Digital Sky Survey \u2013 SDSS)\u00a0 g\u00f6reli olarak dar bir bilimsel ama\u00e7 i\u00e7in tasarlanm\u0131\u015ft\u0131, ancak bu alanlarda \u00e7al\u0131\u015fan gruplardaki gen\u00e7 biliminsanlar\u0131 elde edilen verilerle \u00e7ok geni\u015f ara\u015ft\u0131rma alanlar\u0131 a\u00e7t\u0131lar. SDSS \u00f6rne\u011finde, ara\u015ft\u0131rma verilerinin hepsinin kamuya a\u00e7\u0131k veri taban\u0131 olu\u015fturulmas\u0131yla t\u00fcm d\u00fcnyadaki g\u00f6kbilimcilerin bu verilere ula\u015f\u0131p kendi SDSS projelerini yapmalar\u0131n\u0131 ve ara\u015ft\u0131rma grubunun olanaklar\u0131yla bireysel yarat\u0131c\u0131l\u0131k \u015fans\u0131n\u0131n artmas\u0131n\u0131 sa\u011flad\u0131lar.<\/p>\n

5) Bilimsel bilgiye yap\u0131lan katk\u0131n\u0131n \u00f6d\u00fcl\u00fc o alanda ilk \u00f6ng\u00f6r\u00fcden ve bu \u00f6ng\u00f6r\u00fcn\u00fcn ger\u00e7ekle\u015fmesi \u00e7al\u0131\u015fmas\u0131nda yarat\u0131c\u0131 yanlar\u0131n ortaya \u00e7\u0131kar\u0131lmas\u0131ndan sorumlu olan ki\u015fiye verilmelidir. G\u00fcn\u00fcm\u00fczde, astrofizikte ge\u00e7erli olan de\u011ferlendirme biliminsan\u0131n\u0131n ad\u0131 ge\u00e7en makaleye ald\u0131\u011f\u0131 at\u0131f say\u0131s\u0131yla \u00f6l\u00e7\u00fcl\u00fcyor; ki\u015fi \u00e7al\u0131\u015fman\u0131n tek yazar\u0131 m\u0131 yoksa 165 ki\u015filik yazar listesinin 47. s\u0131ras\u0131ndaki mi \u00f6nemli de\u011fil. Bu durum, yazar ve referans listesinde enflasyonu k\u00f6r\u00fckler, yarat\u0131c\u0131 \u00e7al\u0131\u015fman\u0131n g\u00f6r\u00fcn\u00fcrl\u00fc\u011f\u00fcn\u00fc suland\u0131r\u0131r. Asl\u0131nda suland\u0131rman\u0131n ilk a\u015famas\u0131 b\u00fcy\u00fck gruplar halinde \u00e7al\u0131\u015fmada yat\u0131yor. Bu suland\u0131rmaya kar\u015f\u0131 al\u0131nacak \u00f6nlem makalenin ilk yazar\u0131na daha fazla hak tan\u0131y\u0131p di\u011fer yazarlara normalize edilmi\u015f at\u0131f sunmakla (N yazarl\u0131 makalede di\u011fer yazarlara 1\/N oran\u0131nda at\u0131f hakk\u0131) sa\u011flanabilir. Bu y\u00f6ntem yazar listesindeki enflasyon e\u011filimini engelleyebilir ve her bir astrofizik\u00e7inin bireysel katk\u0131s\u0131na daha adil bir de\u011ferlendirme sa\u011flar. E\u011fer bu yeteneklerin tan\u0131s\u0131n\u0131 uygun bir bi\u00e7imde yapamazsak, o gen\u00e7 ve yarat\u0131c\u0131 astrofizik\u00e7iler ba\u015fka \u00e7al\u0131\u015fma alanlar\u0131na kayabilir.<\/p>\n

6) Astrofizik\u00e7iler etkinliklerini y\u00fcksek erke fizi\u011fi alan\u0131nda de\u011fil, kendi k\u00fclt\u00fcrel ba\u011flamlar\u0131nda ya\u015fama ge\u00e7irmelidir. \u00d6\u011frenci ve gen\u00e7 biliminsanlar\u0131yla etkile\u015fimde bu noktaya \u00f6zellikle dikkat edilmelidir. Karanl\u0131k erkenin b\u00fcy\u00fcleyici bir sorunsal oldu\u011fu yads\u0131namaz, ancak bu y\u00fcksek erke fizi\u011finin sorunsal\u0131d\u0131r. Karanl\u0131k erkenin anla\u015f\u0131lmas\u0131ndaki<\/strong> yarat\u0131c\u0131l\u0131k, planlanm\u0131\u015f g\u00f6kbilim ara\u015ft\u0131rmalar\u0131ndan gelmeyecektir. Planlanm\u0131\u015f g\u00f6kbilim ara\u015ft\u0131rmalar\u0131 astrofizi\u011fin \u00e7ok iyi bildi\u011fi niceliklere ili\u015fkin daha do\u011fru \u00f6l\u00e7\u00fcmler yapacakt\u0131r. S\u00f6z\u00fc edilen g\u00f6zlemlerin do\u011frulu\u011fu temel sorundur, ancak ki\u015fi, devasa veri tabanlar\u0131n\u0131n i\u015flenmesi veya veri \u00e7\u00f6z\u00fcmlemesinin istatisti\u011fiyle ilgilenmezse, bu temel sorun \u00e7ok az bilimsel yarat\u0131c\u0131l\u0131k \u015fans\u0131 sunar.<\/p>\n

\"\"
Avrupa G\u00fcney G\u00f6zlemevi\u2019nde (ESO) ufukta Samanyolu G\u00f6kadas\u0131 y\u00fckselirken, ona e\u015flik eden ba\u015fka g\u00f6kadalarda g\u00f6r\u00fcnt\u00fcye girmi\u015f… (Kaynak: http:\/\/www.eso.org\/)<\/figcaption><\/figure>\n

Parlak ve ihtirasl\u0131 \u00f6\u011frenciler e\u011fer \u00e7al\u0131\u015fma alanlar\u0131nda y\u00fcksek etki yapacak olan bireysel katk\u0131 \u015fans\u0131 g\u00f6r\u00fcrlerse, astrofizik\u00e7i olmaya karar vereceklerdir. Karanl\u0131k erke ara\u015ft\u0131rmalar\u0131nda bu t\u00fcr \u015fans b\u00fcy\u00fck \u00f6l\u00e7\u00fcde g\u00f6kcisimleri \u00fczerinde yap\u0131lacak olan \u00e7al\u0131\u015fmalardan gelecektir. Parasal destek kazanma tela\u015f\u0131yla projeye karanl\u0131k erke etiketi yap\u0131\u015ft\u0131rmak, g\u00f6kbilimi \u201cikincil\u201d \u00f6neme indirmek anlam\u0131na gelir, bu yakla\u015f\u0131m kozmik geni\u015fleme ve b\u00fcy\u00fck yap\u0131lar\u0131n b\u00fcy\u00fcme tarih\u00e7esine ili\u015fkin \u00f6l\u00e7\u00fcmleri daha az \u00f6nemli k\u0131lar.\u00a0 Karanl\u0131k erkenin bir\u00e7ok modelin \u00f6ng\u00f6r\u00fcs\u00fcnden daha karma\u015f\u0131k (veya farkl\u0131) oldu\u011fu ortaya \u00e7\u0131kabilir. Karanl\u0131k erkenin do\u011fas\u0131na ili\u015fkin bu kritik ipucu hassas \u00f6l\u00e7\u00fcmlerden \u00e7ok g\u00f6kada k\u00fcmeleri gibi yap\u0131lara ili\u015fkin geleneksel g\u00f6kbilim ara\u015ft\u0131rmalar\u0131ndan gelebilir.<\/p>\n

G\u00f6kbilim fizik bilimleri aras\u0131nda en eski tarih\u00e7eye sahip oldu\u011funu ileri s\u00fcrer ve e\u011fitilmi\u015f toplumlarda yaratt\u0131\u011f\u0131 k\u00fclt\u00fcrel ve entelekt\u00fcel ilgi di\u011fer fizik dallar\u0131n\u0131nkinden daha fazlad\u0131r. Bu nedenle, bir\u00e7ok \u00fcniversite b\u00f6l\u00fcmleri astronomiyi fizi\u011fin b\u00fcy\u00fck bir davas\u0131n\u0131n temsilcisi veya savunucusu olarak g\u00f6r\u00fcr. G\u00f6kbilim, \u00e7al\u0131\u015fma ve ilgi alan\u0131 bilimsel olmayan kamuya anlayabilece\u011fi bilimsel y\u00f6ntem, \u00f6\u011frencileri de fizi\u011fe \u00e7ekerek geni\u015f bir hizmet alan\u0131 sunar. \u00c7ekicilik g\u00f6kbilimdeki \u00e7e\u015fitlilikten kaynaklan\u0131r. G\u00f6kbilim insan topluluklar\u0131na dolays\u0131z olarak uygulanamaz ancak d\u00fcnyam\u0131z\u0131n ve i\u00e7inde bulundu\u011fumuz evrenin geli\u015fimine ili\u015fkin bilgi da\u011farc\u0131\u011f\u0131yla \u00e7ekicili\u011fini s\u00fcrd\u00fcr\u00fcr. G\u00f6kbilimin bu g\u00fcc\u00fc temel fizi\u011fin de\u011fi\u015fik ve onu tamamlay\u0131c\u0131 yan\u0131n\u0131 olu\u015fturur. Astrofizi\u011fin s\u00fcregelen canl\u0131l\u0131\u011f\u0131 t\u00fcm ger\u00e7e\u011fin alt\u0131nda yatan derin ger\u00e7e\u011fin s\u0131n\u0131rlar\u0131n\u0131 ara\u015ft\u0131r\u0131p bulma yetene\u011finde de\u011fil, evrenimizi ve i\u00e7indeki g\u00f6kcisimlerini olu\u015fturan s\u00fcre\u00e7lere ili\u015fkin a\u00e7\u0131klamalar\u0131yla hem bizim hem de kamunun b\u00fcy\u00fclenmi\u015fli\u011fini s\u00fcrd\u00fcrmesinde yatar.<\/p>\n","protected":false},"excerpt":{"rendered":"

Karanl\u0131k erke yaln\u0131zca g\u00f6kbilim g\u00f6zlemleriyle ara\u015ft\u0131r\u0131labilecek derin ve ilgin\u00e7 bir sorunsald\u0131r. Ancak bu sorunsal bir\u00e7ok ilgin\u00e7 sorunsaldan yaln\u0131zca bir tanesidir ve \u201c\u00e7\u00f6z\u00fcm\u00fc\u201d \u00e7ok d\u00fc\u015f\u00fck olas\u0131l\u0131kla yap\u0131labilecektir. Karanl\u0131k erkenin s\u0131n\u0131rlar\u0131 belirlenebilir, bu konudaki olas\u0131l\u0131klar\u0131n \u00e7o\u011fu d\u0131\u015flanabilir, ancak bir\u00e7o\u011fu da varl\u0131\u011f\u0131n\u0131 s\u00fcrd\u00fcrecektir. Karanl\u0131k erkenin b\u00fcy\u00fcleyici bir sorunsal oldu\u011fu yads\u0131namaz, ancak bu y\u00fcksek erke fizi\u011finin sorunsal\u0131d\u0131r. G\u00f6kbilimciler olarak […]<\/p>\n","protected":false},"author":475,"featured_media":19472,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"_acf_changed":false,"footnotes":""},"categories":[175,30,26],"tags":[248,657,288,1084,356],"class_list":["post-19470","post","type-post","status-publish","format-standard","has-post-thumbnail","hentry","category-138-sayi","category-astronomi","category-fizik","tag-astronomi","tag-evren","tag-fizik","tag-karanlik-madde","tag-parcacik-fizigi"],"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